The nature and distribution of carbon recombination-line emission in the rho Ophiuchi dark cloud

Details The nature and distribution of carbon recombination-line emission in the rho Ophiuchi dark cloud The nature and distribution of carbon recombination-line emission in the rho Ophiuchi dark cloud

Sep 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974apj...192..607b&link_type=abstract

Astrophysical Journal, vol. 192, Sept. 15, 1974, pt. 1, p. 607-614.

Astronomy and Astrophysics

Astrophysics

44

Carbon, Line Spectra, Near Infrared Radiation, Nebulae, Radiative Recombination, B Stars, Electron Density (Concentration), Emission Spectra, Interstellar Matter, Interstellar Radiation, Radio Spectra

Scientific paper

Observations of the C 167 alpha line at two positions and of the C 110 alpha line at six positions in the rho Oph dark cloud show the recombination-line emission to be detectable in a region of about 1 deg in extent. The high-frequency observations suggest that individual emission regions have angular sizes less than 6 min. From a comparison of the C 167 alpha line with the C 110 alpha line it is concluded that the electron density is about 1 per cu cm and the temperature T is less than or equal to 20 K in the recombination-line regions. It is suggested that the most reasonable interpretation of these results is that the lines arise in compact C II regions surrounding B-type stars embedded in the dark cloud. It is likely that these are the same stars that have recently been detected as near-infrared point sources. The detection of 350-micron radiation from these same regions reinforces this interpretation.

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