低频时码信号场强计的研制

介绍了BPC低频时码信号场强计的设计方案和原理,并结合出仪器硬件设计和控制软件框图,该仪器体积小,重量轻,测量精度高,对低频时码系统工程应用和低频电波传播特征研究具有重要意义。     

低频时码接收机的FIR滤波器设计及其DSP实现

将FIR(有限冲击响应)数字滤波器应用于低频时码接收机中,并利用DSP(digital signal proccssor)芯片TMS320C5402实现了低频时码信号的FIR滤波。实验表明,FIR滤波可以使信号中混杂的较为严重的干扰得到很好的抑制,并且失真较小,有利于实现高性能的定时接收机。     

双口RAM在低频时码信号采集系统中的应用

介绍了一种快速双口RAM芯片 IDT7026的结构特点和功能，并将其应用于低频时码信号采集系统中，从而实现了DSP(数字信号处理器)和单片机进行快速数据传输和数据共享的任务。给出了通过该芯片进行DSP和单片机通信的具体接口电路，并针对低频时码信号采集系统中交换数据的仲裁方式，提出了令牌传递和软件判优两种实现方法。     

一种低频时码接收机数字式自动增益控制的设计

为扩大低频时码接收机的输入动态范围,进行了数字式自动增益控制(AGC)的设计。详细介绍了低频时码接收机数字式自动增益控制的设计方法和实现原理,并进行了计算机仿真。仿真结果表明,该数字式自动增益控制是可行的,相对于没有实行自动增益控制的情况而言,大大增加了接收机的动态范围。     

UTC闰秒通知

<正>2015年6月末,协调世界时(UTC)系统将引入1正跳秒。届时,我国综合原子时系统的协调世界时UTC(JATC)和国家授时中心的协调世界时UTC(NTSC),以及BPL、BPM、BPC长短波授时信号和低频时码信号中的UTC时号都将实施跳秒。     

UTC闰秒通知

2008年12月末,协调世界时(UTC)系统将引入1正跳秒。届时,我国综合原子时系统的协调世界时UTC(JATC)、国家授时中心的协调世界时UTC(NTSC)及其所控制的实时时间UTC(NTSC MC),以及BPL、BPM、BPC长短波授时信号和低频时码信号中的UTC时号都将     

UTC闰秒通知

2012年6月末,协调世界时(UTC)系统将引入1正跳秒。届时,我国综合原子时系统的协调世界时UTC(JATC)、国家授时中心的协调世界时UTC(NTSC)及其所控制的实时时间UTC(NTSC MC),以及BPL、BPM、BPC长短波授时信号和低频时码信号中的UTC时号都将实     

UTC闰秒通知

<正>2015年6月末,协调世界时(UTC系统将引入)1正跳秒。届时,我国综合原子时系统的协调世界时UTC(JATC和国家授时中心的协调世界时)UTC(NTSC,以及)BPL、BPM、BPC长短波授时信号和低频时码信号中的UTC时号都将实施跳秒。跳秒前后UTC秒信号所标志的时刻依次为:     

UTC闰秒通知

<正>2015年6月末,协调世界时(UTC系统将引入)1正跳秒。届时,我国综合原子时系统的协调世界时UTC(JATC和国家授时中心的协调世界时)UTC(NTSC,以及)BPL、BPM、BPC长短波授时信号和低频时码信号中的UTC时号都将实施跳秒。     

UTC闰秒通知

<正>2012年6月末,协调世界时(UTC)系统将引入1正跳秒。届时,我国综合原子时系统的协调世界时UTC(JATC)、国家授时中心的协调世界时UTC(NTSC)及其所控制的实时时间UTC(NTSCMC),以及BPL、BPM、BPC长短波授时信号和低频时码信号中的UTC时号都将实     

基于DSP的小型化高精度频标比对系统研制

针对传统双混频时差法测频的局限性,提出了一种差拍数字化精密频率测量方法,基于正弦差拍技术、同步采样技术和数字信号处理技术设计实现了一种新型频标比对系统,可实现对5MHz、10MHz等频标信号的比对测量。实验结果证明,测量10MHz频标信号时系统本底噪声约为1×10^-12／s。系统拥有测量精度高,体积小以及成本低的特点,在时频测量领域具有良好的推广和应用价值。     

YH-1星载超稳定晶振的频率稳定性的测试与分析

中国首个火星探测器萤火1号拟定在2011年发射升空。探测器上配备了一组(2个)超稳定晶体振荡器,该组晶体振荡器为X波段发射机提供频率标准,向地球发射下行信号。地面台站采用无线电开环多普勒和甚长基线干涉测量技术,对其进行通信、导航和跟踪。分析处理了萤火1号的超稳定晶体振荡器频率实验测试数据,确认晶体振荡器的频率稳定度约为1×10~(12),此结果可以作为火星探测器精密测定轨的有力支撑。     

遥测接收机基带信号处理的数字化实现方法

根据VLBI系统中接收的遥测信号基带信号的特点,介绍了利用虚拟无线电技术实现遥测接收机基带信号处理的基本原理,并分别概述了接收机的载波解调、副载波解调、数据转换环3个功能模块的数字化实现方法。仿真结果和实测数据表明,利用虚拟无线电技术能够很好地实现对遥测信号的解调和同步工作,又因该技术本身具有容易更新、方便添加接口、可并行化等优点,这种基于虚拟无线电技术的遥测接收机基带处理系统,将能够为遥测、导航、天线组阵等相关技术提供很好的实验和应用平台。     

Optical fiber positioning based on four-quadrant detector with Gaussian fitting method

With the development of large-scale spectral surveys, fiber positioning technology has been developing rapidly. Because of the performance advantages of a four-quadrant(4Q) detector, a fiber positioning and real-time monitoring system based on the 4Q detector is proposed. The detection accuracy of this system is directly determined by the precision of the center of the spot. A Gaussian fitting algorithm based on the 4Q detector is studied and applied in the fiber positioning process to improve the calculated accuracy of the spot center. The relationship between the center position of the incident spot and the detector output signal is deduced. An experimental platform is built to complete the simulated experiment. Then we use the Gaussian fitting method to process experimental data, compare the fitting value with the theoretical one and calculate the corresponding error.     

Study of Radio Frequency Interference Mitigation Method Based on Wavelet Transform

In radio astronomy observations, radio frequency interference (RFI) is mixed into the telescope receiving system in various forms. The existence of RFI brings misjudgment to the observation or reduces the observational signal-to-noise ratio. In recent years, the domestic and overseas radio astronomy has developed rapidly. Large-scale radio telescopes and telescope arrays at home and abroad have been constructed successively. Observation sensitivity is greatly improved, and the influence of RFI is particularly prominent. With the development of science and technology and the intensification of human activities, the RFI has become increasingly serious and irreversible. We propose to use the two-dimensional discrete wavelet transform method to analyze the data of radio astronomy observations, and to perform wavelet transform on the time-frequency sequence output by the telescope system. According to the wavelet coefficients, the every component in the original signal is separated, and the corresponding threshold value is obtained by the statistics on each component. Each component is compared with the threshold to identify the interference component, and to mark it for removal. This method is used to process the actual observation data. The results show that this method can well mark and eliminate the interference signal, and improve the observational signal-to-noise ratio.     

基于小波变换的射频干扰消除方法的研究

在射电天文观测中,射频干扰(Radio Frequency Interference, RFI)会以多种形式混入望远镜接收系统,给观测带来误判或者降低观测信噪比.近年来国内国际射电天文快速发展,国内国际大型射电望远镜和阵列先后建设,观测灵敏度大为提高,射频干扰的影响尤为突出.随着科技发展和人类活动的加剧,射频干扰日益严重且不可逆转.提出利用2维离散小波变换的方法分析射电天文观测的数据,对望远镜系统输出的时间频率序列进行小波变换,根据小波系数分离出原始信号中各分量,每个分量统计得到相应的阈值,将各分量与阈值相比较识别干扰成分并标记去除.利用该方法对实际观测数据进行了处理,结果表明该方法能够很好地标记并消减干扰信号,且提高了观测的信噪比.     

Antenna data storage concept for phased array radio astronomical instruments

Low frequency Radio Astronomy instruments like LOFAR and SKA-LOW use arrays of dipole antennas for the collection of radio signals from the sky. Due to the large number of antennas involved, the total data rate produced by all the antennas is enormous. Storage of the antenna data is both economically and technologically infeasible using the current state of the art storage technology. Therefore, real-time processing of the antenna voltage data using beam forming and correlation is applied to achieve a data reduction throughout the signal chain. However, most science could equally well be performed using an archive of raw antenna voltage data coming straight from the A/D converters instead of capturing and processing the antenna data in real time over and over again. Trends on storage and computing technology make such an approach feasible on a time scale of approximately 10 years. The benefits of such a system approach are more science output and a higher flexibility with respect to the science operations. In this paper we present a radically new system concept for a radio telescope based on storage of raw antenna data. LOFAR is used as an example for such a future instrument.     

宽带频谱序列干扰信号识别与统计方法

随着科学技术的不断进步,射电天文台站趋于自动化,各类电子设备的广泛使用使得射电天文台站的电磁环境变得尤为复杂,如何有效识别和统计复杂频谱中的干扰信号是当前射电天文台站亟需解决的问题,故提出一种宽带频谱序列干扰信号识别与统计方法.首先,对每组宽带频谱进行信噪分离、识别频谱中的干扰信号;然后,对第1组宽带频谱信号识别结果及信号特征建立模板库,后续每组频谱的信号识别结果与模板库中对应频率的信号进行相似性分析,根据相似性分析结果,统计信号次数,更新模板库;实现宽带频谱序列干扰信号的识别与统计.针对QTT (QiTai Radio Telescope)台站实测频谱,运用该方法进行干扰信号识别与统计,能够有效识别并标记频谱中的干扰信号,并统计干扰信号随时间、方向的变化趋势.     

A high speed networked signal processing platform for multi-element radio telescopes

A new architecture is presented for a Networked Signal Processing System (NSPS) suitable for handling the real-time signal processing of multi-element radio telescopes. In this system, a multi-element radio telescope is viewed as an application of a multi-sensor, data fusion problem which can be decomposed into a general set of computing and network components for which a practical and scalable architecture is enabled by current technology. The need for such a system arose in the context of an ongoing program for reconfiguring the Ooty Radio Telescope (ORT) as a programmable 264-element array, which will enable several new observing capabilities for large scale surveys on this mature telescope. For this application, it is necessary to manage, route and combine large volumes of data whose real-time collation requires large I/O bandwidths to be sustained. Since these are general requirements of many multi-sensor fusion applications, we first describe the basic architecture of the NSPS in terms of a Fusion Tree before elaborating on its application for the ORT. The paper addresses issues relating to high speed distributed data acquisition, Field Programmable Gate Array (FPGA) based peer-to-peer networks supporting significant on-the fly processing while routing, and providing a last mile interface to a typical commodity network like Gigabit Ethernet. The system is fundamentally a pair of two co-operative networks, among which one is part of a commodity high performance computer cluster and the other is based on Commercial-Off The-Shelf (COTS) technology with support from software/firmware components in the public domain.     

Simultaneous estimation of noise and signal in cosmic microwave background experiments

To correctly analyse data sets from current microwave detection technology, one is forced to estimate the sky signal and experimental noise simultaneously. Given a time-ordered data set we propose a formalism and method for estimating the signal and associated errors without prior knowledge of the noise power spectrum. We derive the method using a Bayesian formalism and relate it to the standard methods; in particular we show how this leads to a change in the estimate of the noise covariance matrix of the sky signal. We study the convergence and accuracy of the method on two mock observational strategies and discuss its application to a currently-favoured calibration procedure.