德令哈13.7m望远镜多波束接收机的运行

德令哈13.7 m望远镜是中国最重要的射电望远镜之一.望远镜自安装超导成像频谱仪以及采用飞行观测模式以来,运行近10 yr.在此期间,望远镜开展并完成大量的天文观测,累积了巨量的天文数据,取得了一系列重要的科研成果.介绍了超导成像频谱仪在天文观测中的运行状态,运行中疑难问题、故障现象及解决方案.详述了超导成像频谱仪各方面性能测试及多年来的性能分析,包含接收机噪声温度及望远镜系统噪声温度、镜像抑制比、接收机稳定性、波束性能等方面.列举了超导成像频谱仪更新发展方面的工作,包含本振功率自动化调整、边带分离型超导混频器预放大电路的更新、控制程序的优化等.总结经验和规律,承前启后,将过去的超导成像频谱仪的维护运行经验应用到之后新一代大规模接收机系统中.     

阵列接收系统的噪声温度分析

针对射电天文抗干扰技术对于射电天文观测设备灵敏度的影响,分析了评估自适应波束形成技术对阵列接收系统的噪声温度影响.首先通过噪声信号模型,获取了影响系统噪声温度变化的参数,并在此基础上研究了天线增益、接收机增益和耦合性等系统参数的不确定性对于噪声温度的影响,最后利用仿真实验分析了理想系统条件下当前主要的自适应波束形成算法对于系统噪声温度的影响.结果表明基于自适应波束形成的抗干扰方法在天文信号源和干扰信号源重合的情况下已不再适用.     

S波段双极化低噪声接收机的设计与制作

所述的S波段双极化低噪声接收机是乌鲁木齐天文站根据天文观测研究的需要而设计制作的,接收机采用超外差式结构,设计中对接收机的噪声参数进行了细致地分析和合理地分配,分析选择了符合设计要求的接收机器件,制作中采取有效方法,改善接收机的噪声特性和阻抗匹配,并采用多种测试方法对接收机进行了测试,实测结果与设计分析的指标非常吻合,说明接收机的设计与制作都很成功,接收机噪声温度小于50K,达到国际同类接收机的水平.     

德令哈毫米波望远镜本振谐波干扰问题

射电天文中,射频干扰问题多样而复杂,面对不同的射频干扰问题,针对不同的干扰机制,采取针对性的方法。从器件阶段消减射频干扰,可以预防射频干扰进入望远镜内部。介绍了德令哈毫米波望远镜9波束边带分离型超导接收机, 1个本振链路系统分配18路本振信号方案,针对本振链路中信号发生器的谐波信号引起的中频窄带干扰,设计了注入模拟谐波信号的测试方案,确认了干扰产生机制并得出谐波信号频率与干扰信号频率和功率的对应关系,分析并验证了谐波干扰的传输路径。为了消减谐波干扰,利用YIG滤波器可变频段的带通特性,在本振链路上滤除谐波信号,防止谐波信号耦合到接收机系统,完成了谐波干扰的消减。     

亚毫米波射电天文用超导SIS接收机的研制(英文)

为了研制亚毫米波射电天文用超导SIS(超导 -绝缘体 -超导 )接收机 ,我们重点开展了如下研究 ,1 )Nb超导SIS结在其能隙频率附近的量子混频特性 ,及其结合高能隙超导薄膜 (NbTiN)和高电导率金属薄膜 (Al)分布结阵在 780 - 950GHz频率区间的量子混频特性 ;2 )亚毫米波超导混频器嵌入阻抗的数值和实验表征 ;3)高电流密度小面积Nb超导SIS结的制备和特性表征 ;4)一个 60 0 - 72 0GHz超导SIS混频器的研制和特性表征。本文详细介绍了相关的数值分析和实验测量结果。     

基于斩波轮技术的K波段接收机噪声校准研究

接收机是射电天文中用于探测微弱射电信号的重要接收设备.接收机的强度校准就是将接收机对射电源的响应转换为天文意义上的流量密度.常规方法就是使用经典的冷热负载法,将接收机自身的强度响应转换为一个等效的温度值,之后再据此对射电源做进一步标定.通过搭建基于斩波轮技术的K波段接收机强度校准平台,使用斩波轮法测试K波段常温接收机的噪声温度,并与传统冷热负载法的测试结果进行比对.结果显示,在晴好天气条件下,斩波轮法在30°、90°仰角下噪声温度的最大测试误差为7.5%和8.4%,可以很好地应用于实际噪声温度测试中;但在5°仰角测试中,由于过低仰角引入了地面噪声,使得斩波轮法的测试误差上升至20%–30%之间而无法使用.希望在此基础上进一步开展K波段天空亮温度的理论计算与实测,从而完善斩波轮技术的应用,使之可以满足在不同气象条件下的噪声校准测试需求.     

德令哈13.7m望远镜接收机抗射频干扰研究

在天文观测中,射频干扰会造成假谱,降低数据的可靠性和有效性.射频干扰消减旨在减少干扰信号对射电天文观测的影响,包含器件方面的技术革新和数据处理领域的方法研究.针对德令哈13.7 m望远镜接收机中频部分引入的射频干扰,通过优化中频器件的抗射频干扰能力,提高了接收机的整体抗射频干扰能力,以主动消除方法来减少射频干扰耦合到接收机内部.分析了接收机干扰的传输路径,提出了器件射频干扰的直接耦合系数和器件射频干扰的系统耦合系数的概念,为定位干扰敏感器件并量化干扰引入比重提供了基础.经过抗射频干扰优化后,接收机抗干扰能力改善30 dB左右,望远镜的天文观测效率提高10%以上.     

数字边带分离校准研究

边带分离(Sideband-separating, 2SB)接收可实现上边带(Upper Sideband, USB)和下边带(Lower Sideband, LSB)信号同时观测,观测效率高且上、下两边带不会出现混叠.因此在射电天文观测应用中越来越受到重视.由于全模拟边带分离接收机存在难以克服的幅度和相位误差,导致了边带抑制率较低,影响了系统的性能.数字边带分离接收机可通过数字信号处理方法,有效改善系统边带抑制率.在3–18 GHz频段构建数字边带分离接收机原理实验,并基于边带分离理论和数字校准方法,实现实验系统的边带不平衡度校准,大大改善了系统的边带抑制率.     

基于100 nm砷化镓pHEMT工艺的C波段宽带低噪声放大器芯片

作为射电天文接收机系统的关键器件, 低噪声放大器的噪声和增益性能对接收机系统的灵敏度有重要影响. 采用100nm砷化镓赝配高电子迁移率晶体管(pseudomorphic High Electron Mobility Transistor, pHEMT)\lk工艺, 研制了一款可覆盖C波段(4--8GHz)的低噪声放大器(Low Noise Amplifier, LNA). 所设计的LNA采用3级共源级联放大拓扑结构, 栅极、漏极双电源供电. 常温下测试表明, 该LNA在4--8GHz频段内平均噪声温度为\lk60K, 在5GHz处获得最低噪声温度50K, 通带内增益($31\pm1.5$)dB, 输入输出回波损耗均优于10dB, 芯片面积为$2.1\times1.1$mm², 可以应用于C波段射电天文接收机以及卫星通信系统等.     

2～18 GHz超宽带低噪声放大器芯片研制

低噪声放大器在射电天文望远镜接收机中是一个重要的前端组件,其性能对接收机的灵敏度和噪声有至关重要的影响。采用OMMIC公司70 nm GaAs mHEMT工艺研究和设计了一款工作频率为2～18 GHz的超宽带单片微波集成低噪声放大器芯片,芯片面积为2 mm×1 mm。放大器电路采用三级级联放大、双电源供电拓扑结构,常温在片测试结果显示,全频带增益大于28 dB,噪声温度平均值为93 K,直流功耗150 mW,无条件稳定。该放大器芯片覆盖了射电天文S, C, X, Ku 4个传统观测波段,适用于厘米波段超宽带接收前端和毫米波段超宽带中频放大模块。     

Investigation of LO-Coupled Noise for a Sideband Separation Superconducting SIS Receiver

The Superconducting Superconductor-Insulator-Superconductor (SIS) receivers have become the preferred method for (sub)millimeter-wave radio astronomical observations due to the extremely low receiver noise temperature. The coupling noise of the local oscillator (LO) system is also a part of the receiver noise. In many years of astronomical observations, it is found that the LO-coupled noise cannot be completely ignored, which has a certain impact on the sensitivity of astronomical observations. The noise temperature of the superconducting SIS receiver was tested using two different kinds of signal generators as the primary signal source of the LO system. It is found that the base noise output by the signal generator can be coupled into the receiver to increase the receiver noise. By adding a narrow band filter to the output of the signal generator, the base noise of the signal generator can be filtered out, and this part noise of the receiver can be eliminated, the overall noise of the receiver is reduced, and the sensitivity of the telescope is improved.     

The Operation of Multi-beam Receiver of Delingha 13.7 m Telescope

Delingha 13.7 m telescope is one of the most important radio telescopes in China. Since installing the superconducting spectroscopic array receiver (SSAR) and adopting the On The Fly (OTF) observation mode, the telescope has operated for nearly 10 years. During this period, a large number of astronomical observation projects have been carried out and completed, a large amount of astronomical data have been accumulated, and a series of important scientific results have been achieved. This paper introduces the operating status of SSAR in astronomical observations, the problems in operations, as well as the fault phenomena and solutions. The performance test and performance analysis of SSAR are described in detail, including the receiver noise temperature and telescope system noise temperature, image rejection ratio (IRR), receiver stability, beam performance and so on. The updating and development of SSAR are listed, including the automatic adjustment of LO (Local Oscillator) power, the updating of pre-amplification circuits of the sideband separation superconducting mixer, and the optimization of control program, etc. This paper summarizes the experiences and rules, and connects the past with the future, for applying the experiences of the maintenance and operation of SSAR to the next-generation large-scale receiver system.     

Research on Receiver Anti-RFI of Delingha 13.7 m Telescope

In astronomical observations, the radio frequency interference (RFI) will cause pseudo spectra and reduce the reliability and validity of observational data. The RFI mitigation, which includes many technical innovations of devices and the method studies of data processing, aims at reducing the influence of RFI on the radio astronomical observation. Various efforts were made to improve the anti-RFI capability of the multi-beam receiver (Superconducting Spectroscopic Array Receiver, SSAR) of the Delingha 13.7 m telescope. The interference transmission path was analyzed. The concepts of the device RFI direct coupling coefficient and the device RFI system coupling coefficient were proposed. The proportions of interference introduced in the receiver system by the different devices were quantified, and the interference-susceptible devices in the system were located. After the anti-RFI treatment of the interference-susceptible devices, the anti-RFI capability of the receiver system is improved by 30 dB in average, and the astronomical observation efficiency of the telescope is increased by more than 10%.     

Phase stability of a satellite-VLBI-receiver at 22 GHz

The phase stability of the Radioastron 22 GHz satellite-VLBI-receiver has been studied by measurements. The resulting performance of the receiver in an interferometer system was evaluated. The maximum phase jitter value of 2° due to the receiver causes only marginal degradation for astronomical observations. During observations the requirement of a phase drift value less than 3° in the receiver system can be met after an initial warm-up if the overall ambient temperature changes do not exceed 4°C.     

measurement of noise power spectrum in photon counting PMT's and the effect of the observed (1/f) noise on astronomical photometry

In astronomical photometry, the sensitivity of observations is limited by the dark counts of the photomultiplier tube. In the present work, the effect of dark count noise in photon counting systems is investigated by theory and experimental measurements. Dark counts are considered to be originating from two sources, namely: dc fluctuations and random pulses.Experimental measurements were carried out to determine noise effects in different operating regions of noise dominance. The results provide strong evidence that: in normal operating mode, where the effect of random pulses is dominant, dark counts do not follow Poisson statistics. The observed noise shows strong (1/f) power spectrum, where the observed noise power is found to increase with time of observation.The results are important in photon counting systems operating under dark count limited mode. The conclusions drawn can be useful in obtaining more accurate error estimates and in assessing astronomical photometric observations and data reduction techniques.     

A 22 GHz receiver with high phase stability for radioastron space-VLBI-mission

A space-qualified low-noise 22 GHz receiver for the international space-VLBI mission Radioastron has been constructed. The microwave electronics is realized by using thermally matched hybrid circuits. The most important properties of the receiver are phase stability, sensitivity and reliability. The high sensitivity is due to a cooled low noise HEMT amplifier (LNA). The measured receiver noise temperature is less than 100 K. The phase stability is achieved by compact structure and thermal stabilization. Phase stabilities of better than 0.13°/°C and 0.2°/°C for the receiver and the LNA units are measured, respectively. The calculated reliability of the receiver exceeds the requirement of 0.97 for the three year mission.     

GPS接收机的中频信号处理算法研究

该文对GPS接收机的中频信号处理算法进行了研究,内容主要涉及信号捕获、载波恢复和伪码跟踪3部分,详细分析了信号捕获过程中所采用的匹配滤波器法、快速傅里叶算法(FFT)、锁频环(FLL)、锁相环(PLL)以及延迟锁定环(DLL)的算法原理,并对环路滤波器作了相应的阐述,给出环路对应的递推公式．     

Extracting 21 cm signal by frequency and angular filtering

Extracting the neutral hydrogen(HI) signal is a great challenge for cosmological 21 cm experiments; both the astrophysical foregrounds and receiver noise are typically several orders of magnitude greater than the 21 cm signal. However, the different properties of the 21 cm signal, foreground and noise can be exploited to separate these components. The foregrounds are generally smooth or correlated over the frequency space along a line of sight(Lo S), while both the 21 cm signal and noise vary stochastically along the same Lo S. The foreground can be removed by filtering out the smooth component in frequency space. The receiver noise is basically uncorrelated for observations at different times, hence for surveys it is also uncorrelated in different directions, while the 21 cm signal, which traces the large scale structure, is correlated up to certain scales. In this exercise, we apply Wiener filters in frequency and angular space to extract the 21 cm signals. We found that the method works well. Inaccurate knowledge about the beam could degrade the reconstruction, but the overall result is still good, showing that the method is fairly robust.