Large-scale (CII) 158 micron emission of the Galaxy observed by a balloon-borne telescope

Details Large-scale (CII) 158 micron emission of the Galaxy observed by a balloon-borne telescope Large-scale (CII) 158 micron emission of the Galaxy observed by a balloon-borne telescope

Dec 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990liaco..29..141s&link_type=abstract

In ESA, From Ground-Based to Space-Borne Sub-mm Astronomy p 141-147 (SEE N91-21986 13-89)

Astronomy and Astrophysics

Astronomy

1

Balloon-Borne Instruments, Fabry-Perot Spectrometers, Interstellar Matter, Line Spectra, Milky Way Galaxy, Spectral Emission, Telescopes, Cryogenic Cooling, Galactic Radiation, High Altitude Balloons, Infrared Astronomy, Molecular Clouds, Stellar Radiation

Scientific paper

Strong (CII) emission lines at 158 microns are detected along the galactic plane using a balloon borne infrared telescope equipped with a liquid helium cooled Fabry-Perot spectrometer. The (CII) intensity distribution is quite similar to that of CO12 and also ressembles those of FIR and 5 GHz continuum but is completely different from that of HI 21 cm. The diffuse (CII) emission probably comes from the diffuse regions illuminated by the general interstellar UV radiation field and form as mantles of giant molecular clouds. If most (CII) intensity observed comes from the diffuse C+ regions, the mass the C+ regions is estimated to be more than 410 pct. of that of the molecular gas traced by CO. The total energy of the (CII) line emitted from the inner Galactic disk amounts to 2.8 x 107 Lgalactic mass, or about 0.36 pct. of the total FIR luminosity of the same region.

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