Other
Scientific paper
Aug 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.221..589l&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 221, Aug. 1, 1986, p. 589-598.
Other
13
Astronomical Spectroscopy, Emission Spectra, Hydrogen Clouds, Molecular Gases, Nebulae, Line Spectra, Radio Spectra, Shock Waves, Ultraviolet Radiation
Scientific paper
Emission from the υ = 1-0 S(1) line of molecular hydrogen at 2.122 μm has been found and mapped in the bipolar nebula S106. The emission is extended along an axis running approximately N-S, similar to the radio and mid-infrared emission. More emission is seen from the north lobe than the south, and generally there is an anti-correlation between the H2 and radio emission. In particular, the strongest H2 emission comes from a peak at the outer boundary of the northern radio lobe. The total luminosity in H2 emission can be accounted for completely either by shock excitation driven by mass loss at a rate close to that calculated by other methods, or by ultraviolet excitation by photons from an O9.0 ZAMS star. Emission line ratios in the 2.0 - 2.5 μm region are indeed consistent with a combination of shock- and ultraviolet-excitation mechanisms.
Jameson Richard F.
Longmore Andrew J.
Robson Ian E.
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