Observations of the 157.7 micron (C II) emission from the galactic H II regions W3 and W51

Details Observations of the 157.7 micron (C II) emission from the galactic H II regions W3 and W51 Observations of the 157.7 micron (C II) emission from the galactic H II regions W3 and W51

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...303..638m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 303, April 15, 1986, p. 638-648.

Astronomy and Astrophysics

Astronomy

9

Carbon, H Ii Regions, Infrared Astronomy, Molecular Clouds, Atomic Excitations, Atomic Recombination, Continuous Spectra, Emission Spectra, Far Infrared Radiation, Infrared Spectra, Ionized Gases, Luminosity, Photodissociation

Scientific paper

The 157.7 micron ground-state fine-structure transition of singly ionized carbon was detected from three positions, each in galactic H II region W3 and W51. These findings show that this emission goes beyond the H II regions and the carbon recombination region in each source. In addition these observations establish a lower limit to the luminosity in the 157.7 micron (C II) line of 360 solar luminosity from W3 and 41 solar luminosity from W51. Mechanisms for 157.7 micron-line excitation are discussed, and it is noted that a substantial part of the observed emission originates in the thin carbon recombination line-emitting region which borders on the H II regions and the warm atomic and molecular gas at the surface of neighboring molecular clouds. It is proposed that excitation by electrons present in the diffuse gas surrounding W51 contributes to the extended 157.7 micron (C II) line emission from this region. It was found that the (C II)FIR continuum ratios for W3 and W51 are in agreement with those of other galactic H II regions.

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