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Molecular Ices as Temperature Indicators in the ISM

Published online by Cambridge University Press:  25 April 2016

R. G. Smith ,
G. Robinson  and
A. R. Hyland
R. G. Smith
Affiliation:
Department of Physics, University College, University of New South Wales, Australian Defence Force Academy, Canberra, ACT 2600
G. Robinson
Affiliation:
Department of Physics, University College, University of New South Wales, Australian Defence Force Academy, Canberra, ACT 2600
A. R. Hyland
Affiliation:
Department of Physics, University College, University of New South Wales, Australian Defence Force Academy, Canberra, ACT 2600
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Abstract

Molecular ices are a common component of the dust in many molecular clouds and circumstellar shells. The most abundant molecule, H2O, has several infrared spectral features which have strongly temperature dependent shapes (FWHM) and peak wavelengths. This paper describes how a study of these features, both astronomically and in the laboratory, can lead to constraints on the temperatures of interstellar dust grains. This is demonstrated in part by comparing several astronomical spectra with laboratory spectra of H2O ice.

Type
Galactic and Stellar
Information
Publications of the Astronomical Society of Australia , Volume 10 , Issue 3 , 1993 , pp. 241 - 246
Copyright
Copyright © Astronomical Society of Australia 1993

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