A Q-band two-beam cryogenic receiver for the Tianma Radio Telescope

A Q-band two-beam cryogenic receiver for the Tianma Radio Telescope (TMRT) has been developed, and it uses the independently-developed key microwave and millimeter-wave components operating from 35 to 50GHz with a fractional bandwidth of 35%. The Q-band receiver consists of three parts: optics, cold...

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Bibliographic Details
Published in:Research in astronomy and astrophysics 2018-04, Vol.18 (4), p.44
Main Authors: Zhong, Wei-Ye, Dong, Jian, Gou, Wei, Yu, Lin-Feng, Wang, Jin-Qing, Xia, Bo, Jiang, Wu, Liu, Cong, Zhang, Hui, Shi, Jun, Yin, Xiao-Xing, Shi, Sheng-Cai, Liu, Qing-Hui, Shen, Zhi-Qiang
Format: Article
Language:English
Subjects:
Amplifiers
Assembly
Bandwidths
Circular polarization
Electromagnetic wave filters
Frequency synthesizers
High pass filters
instrumentation: interferometers
Interferometry
Line spectra
methods: observational
Millimeter waves
Mixers
Noise
Optics
Phase shifters
Radio telescopes
Receivers & amplifiers
telescopes
Temperature range
Very long base interferometry
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Summary:A Q-band two-beam cryogenic receiver for the Tianma Radio Telescope (TMRT) has been developed, and it uses the independently-developed key microwave and millimeter-wave components operating from 35 to 50GHz with a fractional bandwidth of 35%. The Q-band receiver consists of three parts: optics, cold unit assembly and warm unit assembly, and it can receive simultaneously the left-handed and right-handed circularly polarized waves. The cold unit assembly of each beam is composed of a feed horn, a noise injection coupler, a differential phase shifter, an orthomode transducer and two low-noise amplifiers, and it works at a temperature range near 20 K to greatly improve the detection sensitivity of the receiving system. The warm unit assembly includes four radio-frequency amplifiers, four radio-frequency high-pass filters, four waveguide biased mixers, four 4-12 GHz intermediate-frequency amplifiers and one 31-38 GHz frequency synthesizer. The measured Q-band four-channel receiver noise temperatures are roughly 30-40 K. In addition, the single-dish spectral line and international very long baseline interferometry (VLBI) observations between the TMRT and East Asia VLBI Network at the Q-band have been successfully carried out, demonstrating the advantages of the TMRT equipped with the state-of-the-art Q-band receiver.
ISSN:1674-4527
DOI:10.1088/1674-4527/18/4/44