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Infrared Properties of Extragalactic HII Complexes

Published online by Cambridge University Press:  30 March 2016

C. M. Telesco
C. M. Telesco*
Affiliation:
Space Science Division, NASA Ames Research Center, Moffett Field, California 94035

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Many galaxies emit significantly more infrared radiation than expected as directly observable photospheric emission. This emission is not restricted solely, or even predominantly, to the galactic nuclei. Rather, where detailed observations exist, they indicate that pronounced emission often originates throughout the disks and especially in the more extended central regions which are distinct from the nuclei. The process which invariably dominates the emission at wavelengths longer than a few microns is radiation from heated dust. At shorter infrared wavelengths, nebular continuum and line radiation, as well as the stellar photospheres, has been observed. In many cases, this emission has been unambiguously associated with HII complexes.

In this review, we focus first on infrared observations of relatively isolated giant HII complexes in the LMC and the spiral arms of M33 and Ml01. We then examine complexes which extend over several kiloparsecs near the galaxian centers. We will not consider the large body of data on extragalactic infrared emission which, although surely relevant to our discussion, is not straightforwardly attributable to HII complexes rather than unusual phenomena in the nuclei (see Rieke and Lebofsky 1979).

Type
Joint Commission Meetings
Information
Highlights of Astronomy , Volume 6: Highlights of Astronomy. As presented at the XVIIIth General Assembly of the IAU, 1982 , 1983 , pp. 619 - 623
Copyright
Copyright © Reidel 1983

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