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Molecular hydrogen and the 2 micron spectrum of NGC 7027
Smith, H. A.; Larson, H. P.; Fink, U.
AA(Arizona, Universit; Steward Observatory, Tucson, Ariz; U.S. Navy, E.O. Hulburt Center for Space Research, Washington, D.C.), AB(Arizona, University, Tucson, Ariz.), AC(Arizona, University, Tucson, Ariz.)
Astrophysical Journal, Part 1, vol. 244, Mar. 15, 1981, p. 835-843. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Emission Spectra, Hydrogen Recombinations, Infrared Astronomy, Molecular Spectra, Planetary Nebulae, Shock Waves, Astronomical Spectroscopy, H Ii Regions, Helium, Line Spectra, Molecular Excitation, Molecular Gases, Monatomic Gases, Shock Fronts, Spectrum Analysis
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The spectrum of the planetary nebula NGC 7027 in the range 1.6-2.5 microns was obtained with a resolution of 1.2 per cm. The presence of molecular hydrogen emission in the v = 1-0 S(1), Q(1), and Q(3) lines is confirmed, and the detection of H2 lines v = 1-0 Q(2), Q(4), S(0), and S(2) is reported. The H2 line strengths, with upper limits for the v = 2-1 band, suggest a model in which the emitting gas is confined to clumps heated by a shock front accompanying an expanding H II region. Emission lines are also detected from atomic hydrogen (Pfund and Brackett series) and from He I and He II.

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