Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.256..528c&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 256, no. 3, June 1, 1992, p. 528-534.
Astronomy and Astrophysics
Astronomy
22
Infrared Astronomy, Interstellar Matter, Molecular Clouds, Photodissociation, Emission Spectra, Hydrogen Ions, Line Of Sight, Stellar Luminosity
Scientific paper
Images are presented of part of the photodissociation region and ionization front in the northern bar of M17, in the infrared lines of H2, H(+), and the 3.28-micron emission feature, a tracer of the edge of the molecular cloud. Spatial coincidence between the 3.28-micron and H2 emission regions is established to within 1 arcsec, which implies a gas density of n greater than 10 exp 5/cu cm. The peak observed surface brightness in the H2 v = 1-0 S(1) line is 1.5 x 10 exp -7 W/sq m per sr and, if a 70 deg inclination to the line of sight is assumed, this intensity implies a density of 10 exp 5/cu cm, from modeling of 1D, uniform-density photodissociation regions. However, the images reveal clumpy structure down to a scale of 2 arcsec, which means that a clumpy two-component photodissociation region model, one component of high density and the other component of lower density, would be the preferred solution. The value of the density determines whether the attenuation of FUV photons is dominated by dust shielding or line shielding. The possible geometry of the region is also discussed.
Brand Peter W. J. L.
Burton Michael G.
Chrysostomou Antonio
Moorhouse Alan
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