Molecular hydrogen in the vicinity of NGC 7538 IRS 1 and IRS 2 - Temperature and ortho-to-para ratio

Details Molecular hydrogen in the vicinity of NGC 7538 IRS 1 and IRS 2 - Temperature and ortho-to-para ratio Molecular hydrogen in the vicinity of NGC 7538 IRS 1 and IRS 2 - Temperature and ortho-to-para ratio

Mar 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...370..228h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 370, March 20, 1991, p. 228-236.

Astronomy and Astrophysics

Astronomy

9

Astronomical Spectroscopy, Early Stars, Hydrogen, Infrared Sources (Astronomy), Star Formation, Emission Spectra, H Ii Regions, Interstellar Matter, Protostars, Stellar Spectra

Scientific paper

Near-infrared spectroscopic observations of the active star-forming region near NGC 7538 IRS 1 and IRS 2 were made. The relative intensities of the v = 1-0 Q(1), Q(3), and Q(5) lines of molecular hydrogen are used to calculate a rotational excitation temperature. Comparison of the measured intensity of the Q(2) transition relative to the intensity of Q(1) and Q(3) permitted the retrieval of the ratio of ortho-to-para hydrogen. It is found that an ortho-to-para ratio of between 1.6 and 2.35 is needed to explain the Q-branch line intensity ratios, depending on the excitation model used. This range in ortho-to-para ratios implies a range of molecular hydrogen formation temperature of approximately 105 K to 140 K.

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