Infrared images of ionized and molecular hydrogen emission in S106

Details Infrared images of ionized and molecular hydrogen emission in S106 Infrared images of ionized and molecular hydrogen emission in S106

May 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...354..242h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 354, May 1, 1990, p. 242-246. Research supported by the Japan Society for t

Astronomy and Astrophysics

Astrophysics

18

Emission Spectra, H Ii Regions, Hydrogen, Infrared Imagery, Ionized Gases, Nebulae, Fabry-Perot Interferometers, Molecular Clouds, Photodissociation, Radio Emission, Spatial Resolution, Star Formation

Scientific paper

High-resolution emission-line images of the central arcminute of S106 in Br-gamma and H2 v = 1-0 S(1) are presented. The high density, together with the low excitation temperature reported earlier for S106, suggests that the origin of the thermal component in the H2 emission measured by Tanaka et al. (1989) is either high-density fluorescence, that is, collisional de-excitation of the UV pumped H2 in photodissociation regions formed on the dense molecular clumps beyond the ionization fronts, or it is radiation from slow shocks driven by the wind from the central source, propagating into the dense clumps. In either case, a novel physical environment is required to understand the observations.

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