ALMA波段9接收机的设计与性能

A. Baryshev, R. Hesper, W. Wild
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引用次数: 2

摘要

阿塔卡马大型毫米波阵列(ALMA)是欧洲、北美和日本之间的合作,在智利5000米的高度建造一个有50多个12米天线的孔径合成望远镜。在完整配置下,ALMA将在30至950 GHz之间的10个波段进行观测,并将为天文学家提供前所未有的毫米和亚毫米波长的灵敏度和空间分辨率。波段9覆盖602-720 GHz,是基线ALMA项目中最高的频段,因此将提供望远镜最高的空间分辨率。本文介绍了用于阿塔卡马大型毫米波阵列(ALMA)的波段9接收筒的设计。这些是现场可更换外差前端,提供高灵敏度,602-720 GHz频率覆盖,4-12 GHz中频带宽和高准光效率。我们特别关注基于J.R.塔克理论的SIS混频器微波设计计算。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
ALMA Band 9 receiver design and performance
The Atacama Large Millimeter Array (ALMA) is a collaboration between Europe, North America, and Japan to build an aperture synthesis telescope with more than 50 12-m antennas at 5000 m altitude in Chile. In its full configuration, ALMA will observe in 10 bands between 30 and 950 GHz, and will provide astronomers with unprecedented sensitivity and spatial resolution at millimetre and sub-millimetre wavelengths. Band 9, covering 602-720 GHz, is the highest frequency band in the baseline ALMA project, and will thus offer the telescope's highest spatial resolutions. This paper describes the design of the Band 9 receiver cartridges for the Atacama Large Millimeter Array (ALMA). These are field-replaceable heterodyne front-ends offering high sensitivities, 602-720 GHz frequency coverage, 4-12 GHz IF bandwidths, and high quasioptical efficiencies. We specifically focus on the SIS mixer microwave design calculations that are based on J.R. Tucker theory.
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