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Continuum Wavelength Emission from Embedded, Young, and Massive Stellar Objects Beyond 1 μm

Published online by Cambridge University Press:  08 February 2017

Thomas Henning  and
Werner Pfau
Thomas Henning
Affiliation:
Jena University Observatory Schiller gäßchen 2 6900 Jena GDR
Werner Pfau
Affiliation:
Jena University Observatory Schiller gäßchen 2 6900 Jena GDR

Abstract

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One of the components of the galactic infrared background (GIRB) radiation is emission by warm dust grains heated by OB stars embedded in molecular clouds. The main contributors are compact HII regions and comparatively radioquiet infrared (IR) point sources such as the Becklin-Neugebauer object. We present the average energy distribution between 1 and 1300 μm for a sample of BN-type objects. The average color temperature between 60 and 100 μm is ~40 K, which is very similar to the color temperature of the observed warm galactic dust emission (WGDE).

Type
II. Galactic Background Starlight from UV to IR: Observations and Models
Information
Symposium - International Astronomical Union , Volume 139: The Galactic and Extragalactic Background Radiation , 1990 , pp. 113 - 114
Copyright
Copyright © Kluwer 1990 

References

REFERENCES

Chini, R., Krügel, E., and Wargau, W. 1987, Astron. Astrophys., 181, 378.Google Scholar
Cox, P., Krügel, E., and Mezger, P.G. 1986, Astron. Astrophys., 155, 380.Google Scholar
Cox, P., and Mezger, P.G. 1989, Astron. Astrophys. Rev., 1, 49; CM.Google Scholar
Henning, Th., and Gürtler, J. 1986, Astrophys. Space Sci., 128, 199.CrossRefGoogle Scholar
Henning, Th., Pfau, W., and Altenhoff, W. 1989, Astron. Astrophys., in press.Google Scholar
Leisawitz, D., and Hauser, M.G. 1988, Astrophys. J., 332, 954.Google Scholar
Pfau, W., Henning, Th., and Chini, R. 1989, in preparation.Google Scholar