Observations of 2 micron molecular hydrogen emission from NGC 2071, Cepheus A, and GL 961

Details Observations of 2 micron molecular hydrogen emission from NGC 2071, Cepheus A, and GL 961 Observations of 2 micron molecular hydrogen emission from NGC 2071, Cepheus A, and GL 961

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...257..612b&link_type=abstract

Astrophysical Journal, Part 1, vol. 257, June 15, 1982, p. 612-619.

Astronomy and Astrophysics

Astrophysics

66

Emission Spectra, Hydrogen, Infrared Spectra, Interstellar Gas, Molecular Clouds, Molecular Spectra, Carbon Monoxide, H Lines, Main Sequence Stars, Molecular Gases, Red Shift, Spectral Line Width, Stellar Evolution

Scientific paper

The IR emission line at 2.12 microns from the v = 1-0 S(1) transition of H2 has been detected and partially mapped in the vicinity of the high-velocity molecular flows associated with NGC 2071, Cepheus A, and GL 961. The H2 emitting regions for these three sources are extended on a scale of at least 0.2-0.3 pc, comparable to or somewhat greater than the size of the Orion H2 source. The H2 surface brightness, uncorrected for possible extinction, is at least an order of magnitude lower in NGC 2071, Cep A, and GL 961 than in Orion. In NGC 2071 and Cep A, the strongest H2 emission occurs on the side of the central IR source, where the blueshifted CO wings are the prominent component. This fact, combined with higher spectral resolution observations which show asymmetric line profiles with enhanced blueshifted emission, lends support to outflow models for the gas where redshifted H2 emission originates on the far side of the source and experiences greater extinction than blueshifted emission.

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