Development of a Front End Array for Broadband Phased Array Receiver

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外文摘要：The receiver is a signal receiving device placed at the focus of the telescope.In order to improve the observation efficiency,the concept of phased array receiver has been proposed in recent years,which places a small phased array at the focal plane of the reflector,and flexible pattern and beam scanning functions can be achieved through a beamforming network.If combined with the element multiplexing,all beams within the entire field of view can be observed simultaneously to achieve continuous sky coverage.This article focuses on the front-end array of phased array receiver at 0.7-1.8 GHz for QiTai Telescope,and designs a Vivaldi antenna array of PCB structure with dual line polarization.Each polarization antenna is designed to arrange in a rectangle manner by 11 x 10.Based on the simulation results of the focal field,32,18,and eight elements were selected to form one beam at 0.7,1.25,and 1.8 GHz.An analog beamforming network was constructed,and the measured gains of axial beam under uniform weighting were 19.32,13.72,and 15.22 dBi.Combining the beam scanning method of reflector antenna,the pattem test of different position element sets required for PAF beam scanning was carried out under independent array.The pattern optimization at 1.25 GHz was carried out by weighting method of conjugate field matching.Compared with uniform weighting,the gain,sidelobe level,and main beam direction under conjugate field matching have been improved.Although the above test and simulation results are slightly different,which is related to the passive array and laboratory testing condition,the relevant work has accumulated experience in the development of the front-end array for the phased array receiver,and has good guiding significance for future performance verification after the array is installed on the telescope.

外文关键词：

telescopesinstrumentation:detectorstechniques:radar astronomy

作者：

Kai Wang、Liang Cao、Jun Ma、Xue-Feng Duan、Hao Yan、Mao-Zheng Chen、Yun-Wei Ning

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作者单位：

Xinjiang Astronomical Observatory,Chinese Academy of Sciences,Urumqi 830011,China

University of the Chinese Academy of Sciences,Beijing 100049,China

Xinjiang Key Laboratory of Microwave Technology,Urumqi 830011,China

基金：

National Key R&D Program of ChinaNational Natural Science Foundation of ChinaChinese Academy of Sciences(CAS)"Light of West China"ProgramNatural Science Foundation of Xinjiang Uygur Autonomous RegionNatural Science Foundation of Xinjiang Uygur Autonomous RegionResearch on the science and technology partnership program and international science and technology cooperation program of SOperation,Maintenance and Upgrading Fund for Astronomical Telescopes and Facility InstrumentsMinistry of Finance of China(MOF)Chinese Academy of Sciences

项目编号：

2022YFC2205303119730782020-XBQNXZ-0182022D01A3582022D01A1572020E01041

出版年：

2024

DOI：

10.1088/1674-4527/ad24f6

天文和天体物理学研究

中国科学院国家天文台

天文和天体物理学研究

CSTPCD

影响因子：0.406

ISSN：1674-4527

年,卷(期)：2024.24(4)