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International Journal of Infrared and Millimeter Waves

A 40 GHz band SIS receiver using Nb/Al?AlOx/Nb array junctions

Masato Tsuboi, Junji Inatani, Takashi Kasuga, Ryohei Kawabe, Akira Sakamoto, Hiroyuki Iwashita, Kazuhiko Miyazawa

Published Jan 1, 1987• 4 citations
Publisher
DOI
10.1007/bf01010641

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Abstract The authors developed a dual‐frequency (40/100 GHz) SIS receiver with SIS quasi‐particle tunneling junction element as the mixer, for use in the millimeter‐wave array at Nobeyama Radio Observatory, National Astronomical Observatory. The SIS element used is an array composed of four series‐connected Nb/Al‐AlOx/Nb junctions. The receiver is refrigerated to 4.3 K by a closed‐cycle He refrigerator. The receiver realized a very low receiver noise temperature for a wideband, such as 50 to 80 K for 43 to 49 GHz, and 60 to 100 K for 86 to 115 GHz. A wide dynamic range is also realized. At 40 Ghz, the saturation noise temperature is 2000 to 3000 K, compared with the wideband noise. These results indicate that the SIS array element can effectively improve the mixer saturation level without degrading the receiver performance.

Electronics and Communications in Japan (Part II Electronics)•Jan 1, 1989•1 citation
As the Atacama Large Millimeter/submillimeter Array (ALMA) nears completion, 73 dual-polarization receivers have been delivered for each of Bands 3 (84-116 GHz) and 6 (211-275 GHz). The receivers use sideband-separating superconducting Nb/Al-AlOx/Nb tunnel-junction (SIS) mixers, developed for ALMA to suppress atmospheric noise in the image band. The mixers were designed taking into account dynamic range, input return loss, and signal-to-image conversion (which can be significant in SIS mixers). Typical SSB receiver noise temperatures in Bands 3 and 6 are 30 and 60 K, respectively, and the image rejection is typically 15 dB.
Abstract The authors developed a dual‐frequency (40/100 GHz) SIS receiver with SIS quasi‐particle tunneling junction element as the mixer, for use in the millimeter‐wave array at Nobeyama Radio Observatory, National Astronomical Observatory. The SIS element used is an array composed of four series‐connected Nb/Al‐AlOx/Nb junctions. The receiver is refrigerated to 4.3 K by a closed‐cycle He refrigerator. The receiver realized a very low receiver noise temperature for a wideband, such as 50 to 80 K for 43 to 49 GHz, and 60 to 100 K for 86 to 115 GHz. A wide dynamic range is also realized. At 40 Ghz, the saturation noise temperature is 2000 to 3000 K, compared with the wideband noise. These results indicate that the SIS array element can effectively improve the mixer saturation level without degrading the receiver performance.