Comparison of 2.1 and 3.8 micron line profiles of shocked H2 in the Orion molecular cloud

Details Comparison of 2.1 and 3.8 micron line profiles of shocked H2 in the Orion molecular cloud Comparison of 2.1 and 3.8 micron line profiles of shocked H2 in the Orion molecular cloud

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...302..693g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 302, March 15, 1986, p. 693-700. NSF-supported research.

Astronomy and Astrophysics

Astronomy

25

Hydrogen, Infrared Astronomy, Line Spectra, Molecular Clouds, Orion Nebula, Shock Waves, Calibrating, Carbon Monoxide, Gas Flow, Scattering Cross Sections, Spectrum Analysis

Scientific paper

Velocity profiles of the 2.12 μm 1-0 S(1) and 3.81 μm 1-0 O(7) lines of H2 have been measured at a number of locations in the shocked gas region of the Orion molecular cloud. In the center of this region, the O(7) lines have relatively stronger wings than do the S(1) lines. With respect to the velocity of the molecular cloud, blueshifted O(7) emission is more prominent than redshifted emission, as is the case for the S(1) line. These data imply that although some extinction through the outflow is present, the asymmetries in the H2 lines are due in part to actual line-of-sight distributions of velocities within the shocked gas. These distributions appear consistent with the sense of the bipolar outflow observed in millimeter CO lines between the lobes of H2 line emission. Scattering of H2 line photons off moving dust grains apparently is not the major cause of the broadline emission within the lobes.

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