Carbon radio recombination line observations of W3

Details Carbon radio recombination line observations of W3 Carbon radio recombination line observations of W3

Mar 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...174..232r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 174, no. 1-2, March 1987, p. 232-238. Research supported by the Stichting Astr

Astronomy and Astrophysics

Astrophysics

14

Carbon, Molecular Clouds, Nebulae, Radiative Recombination, Radio Emission, Astronomical Maps, Centimeter Waves, H Ii Regions, Interferometry, Line Spectra, Oxygen Recombination, Stimulated Emission

Scientific paper

The H II complex W3 has been observed with a 13arcsec.4×14arcsec.2 angular resolution and 2 km s-1 velocity resolution in the C 166α radio recombination line. These are the first interferometric C 166α observations. The distribution of the emission and the velocity structure seem to support the suggestion that at frequencies as low as 21 cm, only emission from a cold cloud in front of the H II region is observed. In agreement with earlier studies the main contributing emission mechanism is most likely stimulated emission. Structural correlations between the carbon emission and high-resolution radio continuum radiation as well as [O III] emission are discussed, as well as the relation between the carbon cloud and the W3 molecular cloud.

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