H2 emission as a tracer of molecular hydrogen: Large-scale observations of Orion

Details H2 emission as a tracer of molecular hydrogen: Large-scale observations of Orion H2 emission as a tracer of molecular hydrogen: Large-scale observations of Orion

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...436l.185l&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 436, no. 2, p. L185-L188

Astronomy and Astrophysics

Astrophysics

24

Emission Spectra, H Lines, Hydrogen, Molecular Clouds, Orion Nebula, Star Formation, Stellar Winds, Ultraviolet Radiation, Brightness Distribution, Luminosity, Molecular Excitation

Scientific paper

We have detected extremely extended (greater than 1.5 deg, or 12 pc) near-infrared H2 line emission from the Orion A molecular cloud. We have mapped emission in the 1.601 micrometer(s) upsilon = 6 - 4 Q(1) and 2.121 micrometer(s) upsilon = 1 - 0 S(1) lines of H2 along a approx. 2 deg R.A. cut and from a 6' x 6' region near theta1 Ori C. The surface brightness of the extended H2 line emission is 10-6 to 10-5 ergs/s/sq. cm/sr. Based on the distribution and relative strengths of the H2 lines, we conclude that UV fluorescene is most likely the dominant H2 emission mechanism in the outer parts of the Orion cloud. Shock-heated gas does not make a major contribution to the H2 emission in this region. The fluorescent component of the total H2 upsilon = 1 - 0 S(1) luminosity from Orion is 30-40 solar luminosity. Molecular hydrogen excited by UV radiation from nearby OB stars contributes 98%-99% of the global H2 line emission from the Orion molecular cloud, even though this cloud has a powerful shock-excited H2 source in its core. The ability to detect large-scale H2 directly opens up new possibilities for the study of molecular clouds.

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