A determination of the reddening of the H2 emission from the Orion molecular cloud

Details A determination of the reddening of the H2 emission from the Orion molecular cloud A determination of the reddening of the H2 emission from the Orion molecular cloud

Jun 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...230l.175s&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 230, June 15, 1979, p. L175-L178.

Astronomy and Astrophysics

Astrophysics

40

Hydrogen Clouds, Infrared Spectra, Interstellar Extinction, Line Spectra, Astronomical Models, Astronomical Spectroscopy, Molecular Spectra, Radiant Flux Density

Scientific paper

The V = 1 to 0 S(0), S(1), S(2), Q(2), Q(3), Q(4), Q(5), O(5), O(6), and O(7) quadrupole lines of molecular hydrogen from Orion southeast of BN have been observed in order to measure the extinction to the emitting region. From the relative line strengths it is found that the lines are strongly reddened, leading to the conclusion that the source of emission lies deep with the Orion molecular cloud. The visual extinction to the H2 derived from the ratios of S and Q lines is Au = 40 + or - 6; the O(5) and O(6) lines appear to undergo additional extinction beyond that predicted by the van de Hulst reddening curve.

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