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Proceedings Paper

The U.C. Berkeley Space Sciences Laboratory and Department of Physics Submillimeter Receiver
Author(s): A. I. Harris; D. T. Jaffe; R. Genzel
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Paper Abstract

The UCB submillimeter heterodyne receiver is a complete system for high resolution astronomical spectroscopy in the 350 pm and 450 pm atmospheric windows. This compact system mounts directly at the Cassegrain focus of large optical and infrared telescopes. It consists of a laser local oscillator, open structure mixer, quasi-optical coupling system, a broad band IF system, and an acousto-optical spectrometer. The local oscillator is a one meter long submillimeter laser optically pumped by a CO2 laser. The mixer is a quasi-optical corner cube antenna structure and Schottky diode. We currently operate the mixer at room temperature and are evaluating mixer performance at 77 K. The system noise temperature is less than 7000 K SSB during observations. The coupling optics allow efficient use of LO power and result in measured telescope beam efficiencies of 0.40 to 0.45. The instantaneous IF bandwidth of 1.2 GHz (450 km/s at 800 GHz) is well suited for observations of astronomically interesting broad emission lines (e.g. from the Galactic center and outflows). The back end spectrometer is a 1200 x 1 MHz channel dual acousto-optical spectrometer (0.38 km/s resolution at 800 GHz). Most of the recent work with this receiver has been on the CO J=7→6 transition at 806.6517 GHz.

Paper Details

Date Published: 21 April 1986
PDF: 5 pages
Proc. SPIE 0598, Instrumentation for Submillimeter Spectroscopy, (21 April 1986); doi: 10.1117/12.952339
Show Author Affiliations
A. I. Harris, University of California (United States)
D. T. Jaffe, University of California (United States)
R. Genzel, University of California (United States)

Published in SPIE Proceedings Vol. 0598:
Instrumentation for Submillimeter Spectroscopy
Erik L. Kollberg, Editor(s)

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