Low Noise mm-Wave Receivers

Kollberg, E.

doi:10.1109/euma.1980.332804

Cited by 6 publications

(1 citation statement)

References 24 publications

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“…For long millimeter waves low noise receivers have been constructed using maser amplifiers (s 40 GHz) while for shorter wavelengths cooled Schottky diode mixers have successfully been utilized [1]. Since 1979 it has been evident that a superconducting quasiparticle mixer is an attractive alternative, which may offer almost as low noise temperatures as the maser but a larger flexibility concerning bandwidth and tunability.…”

Section: Introductionmentioning

confidence: 99%

A Very Low Noise Quasiparticle (SIS) Mixer Receiver for Radio Astronomical Applications

Olsson¹,

Rudner

Kollberg³

et al. 1982

1982 12th European Microwave Conference

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A Superconducting quasiparticle mixer receiver for 35-50 GHz is described. An array of six Pb In-oxide-Pb 7Bi 3 tunnel junctions with 40 Q array normal resistance and a shunt capacitance of 0.2 pF is used.The mixer is immersed into liquid helium and operated at 2 K. A 3.7-4.2 GHz parametric amplifier, also at 2 K is used as the if amplifier. The high if frequency allows single sideband operation with a system noise temperature of 140 K at 47 GHz. A lens guide is used for guiding the signal from the Cassegrain telescope focus to the liquid helium cooled lens corrugated horn and the mixer. The SSB system noise temperature varies rather smoothly from t 220 K at 35 GHz to b 140 K at 50 GHz suggesting that quantum gain effects are becoming more important at the high frequency end. The receiver is operational in the 20 m mm-wave telescope at the Onsala Space Observatory.

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Section: Introductionmentioning

confidence: 99%