A 15 Element Focal Plane Array for 100 GHz

Neal R. Erickson; Paul F. Goldsmith; G. Novak; Ronald M. Grosslein; P. J. Viscuso; Ronna B. Erickson; C. Read Predmore

doi:10.1109/22.108317

A 15 Element Focal Plane Array for 100 GHz

Neal R. Erickson, Paul F. Goldsmith, G. Novak, Ronald M. Grosslein, P. J. Viscuso, Ronna B. Erickson, C. Read Predmore

Physics and Astronomy

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87 Scopus citations

Abstract

A focal plane imaging array receiver is described which covers the 86–115 GHz frequency range for radio astronomical observations. The 3x5 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.

Original language	English (US)
Pages (from-to)	1-11
Number of pages	11
Journal	IEEE Transactions on Microwave Theory and Techniques
Volume	40
Issue number	1
DOIs	https://doi.org/10.1109/22.108317
State	Published - Jan 1992

ASJC Scopus subject areas

Radiation
Condensed Matter Physics
Electrical and Electronic Engineering

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10.1109/22.108317

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title = "A 15 Element Focal Plane Array for 100 GHz",

abstract = "A focal plane imaging array receiver is described which covers the 86–115 GHz frequency range for radio astronomical observations. The 3x5 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.",

author = "Erickson, {Neal R.} and Goldsmith, {Paul F.} and G. Novak and Grosslein, {Ronald M.} and Viscuso, {P. J.} and Erickson, {Ronna B.} and Predmore, {C. Read}",

note = "Funding Information: Manuscript received February 25, 1991; revised July 1, 1991. The Five College Radio Astronomy Observatory is operated with support from the National Science Foundation under grant AST-88 15406 and with permission of the Metropolitan District Commission of Massachusetts. This work is contribution No. 762 of the Five College Astronomy Department.",

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T1 - A 15 Element Focal Plane Array for 100 GHz

AU - Erickson, Neal R.

AU - Goldsmith, Paul F.

AU - Novak, G.

AU - Grosslein, Ronald M.

AU - Viscuso, P. J.

AU - Erickson, Ronna B.

AU - Predmore, C. Read

N1 - Funding Information: Manuscript received February 25, 1991; revised July 1, 1991. The Five College Radio Astronomy Observatory is operated with support from the National Science Foundation under grant AST-88 15406 and with permission of the Metropolitan District Commission of Massachusetts. This work is contribution No. 762 of the Five College Astronomy Department.

PY - 1992/1

Y1 - 1992/1

N2 - A focal plane imaging array receiver is described which covers the 86–115 GHz frequency range for radio astronomical observations. The 3x5 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.

AB - A focal plane imaging array receiver is described which covers the 86–115 GHz frequency range for radio astronomical observations. The 3x5 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.

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A 15 Element Focal Plane Array for 100 GHz

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