CaltechAUTHORS
  A Caltech Library Service

Submillimeter Wave Astronomy

Werner, M. W. (1976) Submillimeter Wave Astronomy. In: 1976 International Conference on Submillimeter Waves and Their Applications. IEEE , Piscataway, NJ, pp. 96-97. ISBN 9781509031832. https://resolver.caltech.edu/CaltechAUTHORS:20210211-151615899

[img] PDF - Published Version
See Usage Policy.

309kB

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20210211-151615899

Abstract

Scientific Overview. Astronomical observations at submillimeter wavelengths, between 40 μm and 1 mm, study astro-physical sources and problems which differ from and complement those accessible at other wavelengths. Although a few nonthermal sources are known, most of the radiation observed in this spectral band from astronomical sources outside of the solar system comes from extended clouds of gas and dust with temperatures in the range 10-500 K and densities between 10 and 10⁶ atoms cm⁻³. The submillimeter radiation consists of both continuous emission from the sub-micron sized dust particles, which make up ∼ 1% of the total mass, and line emission from atomic and molecular species in the gas. The energy radiated at submillimeter wavelengths is generally supplied to such a cloud in the form of ultraviolet, optical, or near infrared radiation from stars or other luminous objects which is absorbed by the dust and goes into heating the dust and gas. Since only a small amount of dust is required to convert ultraviolet and optical radiation into submillimeter radiation, there are many astronomical sources from which most or all of the observed energy lies in this spectral region, although the objects which heat the dust and gas differ from one submillimeter source to another. Thus intense submillimeter radiation is seen from the center of our Galaxy [1] and from diffusely distributed matter within the galactic plane [2], where the heating is probably due to normal stars; from the nuclei of several other galaxies [3], where exotic heating sources may be important; and from shells of dust and gas which are expelled from and heated by evolving stars [4].


Item Type:Book Section
Related URLs:
URLURL TypeDescription
https://doi.org/10.1109/icswa.1976.9350008DOIArticle
Additional Information:© 1976 IEEE. Work supported by National Aeronautics and Space Administration grants NGL 05 002 207 and NGR 05 002 281.
Funders:
Funding AgencyGrant Number
NASANGL 05 002 207
NASANGR 05 002 281
Record Number:CaltechAUTHORS:20210211-151615899
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20210211-151615899
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:108013
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:12 Feb 2021 15:03
Last Modified:12 Feb 2021 15:03

Repository Staff Only: item control page