Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...252..250h&link_type=abstract
Astrophysical Journal, Part 1, vol. 252, Jan. 1, 1982, p. 250-268. NSF-USAF-supported research.
Astronomy and Astrophysics
Astronomy
94
Astronomical Maps, Infrared Astronomy, Nebulae, Star Distribution, Star Formation, Angular Resolution, Contours, Hydroxyl Emission, Infrared Imagery, Infrared Telescopes, Radio Sources (Astronomy), Stellar Luminosity, Water Masers
Scientific paper
A fast-mapping technique, developed for use on the Wyoming Infrared Telescope, has been used to make infrared images of regions of star formation. We present 10 μm and 20 μm images of Mon R2, W51 IRS 1 and IRS 2, S140, and NGC 7538; and 5 μm images of W51 IRS 2 and NGC 7538. The maps have angular resolutions approaching the Rayleigh limit of the 2.3 m telescope and have a sensitivity to extended sources which is as good as or better than previous observations of the same regions.
The most luminous infrared sources are associated with radio continuum sources and, for these objects, the radio and 20 μm contours bear a remarkable similarity to one another. We also find qualitative support in the cases of W51 IRS 1, and Mon R2 IRS 1, for the blister model of H II regions, in which the exciting source is relatively well separated from the peak radio and infrared emission.
The low-luminosity infrared sources are either not coincident with radio emission or are weak radio sources. This is either because the embedded exciting sources are relatively low luminosity late-type stars which emit relatively few ionizing photons or are surrounded by thick dust shells which block the ionizing flux from the interstellar medium.
The observational technique also provides highly accurate positional information for the objects observed, and we make positional comparisons between near-infrared objects, radio continuum sources, OH and H2O masers, and far-infrared sources.
We conclude that, in several cases, the OH and H2O masers may be at relatively large distances (1017 - 1018 cm) from their primary sources.
Gehrz Robert D.
Grasdalen Gary L.
Hackwell John A.
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