Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989esasp.290..517p&link_type=abstract
In ESA, Infrared Spectroscopy in Astronomy p 517-520 (SEE N90-19084 11-89)
Astronomy and Astrophysics
Astronomy
2
Fluorescence, Galaxies, Hydrogen Clouds, Near Infrared Radiation, Star Formation, Emission Spectra, Galactic Structure, Molecular Clouds, Star Clusters
Scientific paper
Near infrared molecular hydrogen emission, detected from the central star forming complexes in nearby spiral galaxies, are presented. In all cases, measurement of several transitions demonstrates that the bulk of the line emitting gas is excited by ultraviolet radiation, and not by shocks. For most galaxies, the ratio of the molecular (v=1-0 S(1)) to atomic (Br gamma) hydrogen line strengths can be quantitatively understood, the emitting regions are supposed to consist of individual hot stars (or small clusters) embedded within the parent molecular clouds or forming blisters at their surface. Large central star clusters may account for the handful of galaxies which display relatively weak H2 emission.
Hawarden Tim
Mountain Matt
Puxley Phil
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