IEEE Transactions on Microwave Theory and Techniques · 1992 · 76 citations · 8 references
EngineeringElectrical EngineeringPhysicsMicroelectronicsMicrowave EngineeringRadio AstronomyHigh-frequency Semiconductor DevicesMicrowave Integrated CircuitsMicrowave OscillatorsRadio-frequency Integrated CircuitsReceiver SystemsArray DesignCryogenic ReceiversDiode MixersFocal Plane ArraysNoise TemperatureReceiver ArchitectureReceiver NoiseReceiver Noise Temperature
A focal plane imaging array receiver is described which covers the 86-115 GHz frequency range for radio astronomical observations. The 3*5 element array uses cryogenic Schottky diode mixers with integrated HEMT IF amplifiers. A cold quasi-optical filter selects the desired sideband, and terminates the image at 20 K. Polarization interleaving is used to minimize the array size on the sky. LO power is provided by a frequency tripled YIG tuned oscillator. The average receiver noise temperature of the array pixels varies from 250-350 K SSB depending on the frequency. Only three mechanical tuners are used in the system and all functions are under computer control.< <ETX xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">></ETX>
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