The UCB/MPE Cassegrain Submillimeter Heterodyne Spectrometer

Details The UCB/MPE Cassegrain Submillimeter Heterodyne Spectrometer The UCB/MPE Cassegrain Submillimeter Heterodyne Spectrometer

Aug 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987ijimw...8..857h&link_type=abstract

International Journal of Infrared and Millimeter Waves (ISSN 0195-9271), vol. 8, Aug. 1987, p. 857-883. Research supported by th

Physics

Optics

35

Astronomical Spectroscopy, Atmospheric Windows, Carbon Dioxide Lasers, Cassegrain Optics, Heterodyning, Submillimeter Waves, Acousto-Optics, Calibrating, Mixing Circuits, Optical Paths, Radio Astronomy, Schottky Diodes

Scientific paper

The UCB/MPE Submillimeter Heterodyne Spectrometer is a system for astronomical spectroscopy in the high-frequency atmospheric windows from 500 to 1000 GHz. It contains a molecular laser local oscillator, a cooled Schottky open structure mixer, a quasi-optical coupling system, and an acoustooptical spectrometer. The compact receiver mounts at the Cassegrain focus of large infrared astronomical telescopes. The receiver noise temperature on the telescope is approximately 3500 K (DSB) during observations of the CO J = 7-6 line at 806.652 GHz. The spectrometer's frequency resolution and instantaneous bandwidth (less than 2 MHz resolution across 1.1 GHz) are well suited for observations of molecular emission lines from a variety of astronomical sources.

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