Large-scale interaction of the H II region and the quiescent gas in Orion A

Details Large-scale interaction of the H II region and the quiescent gas in Orion A Large-scale interaction of the H II region and the quiescent gas in Orion A

Oct 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...264..592r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 264, no. 2, p. 592-609.

Astronomy and Astrophysics

Astrophysics

30

Cosmic Gases, H Ii Regions, Interstellar Matter, Orion Nebula, Gas Density, Molecular Gases, Spatial Distribution

Scientific paper

Large-scale high-angular-resolution mapping of the Orion A molecular cloud in the J = 12-11, J = 16-15, and J = 24-23 lines of HC3N is reported. Besides the molecular ridge, the large-scale maps show new long and thin molecular filaments (MFs) and 'complex' condensations (CCs). All MFs emerge from the molecular ridge and extend to the west. Their typical H2 densities, kinetic temperatures, and masses are about 100,000/cu cm, about 40 K, and 10-30 solar masses, respectively. Most of the MFs exhibit a velocity gradient of 1-2 km/s pc along their length. Though the HC3N abundance is fairly constant (about 10 exp -9) for the molecular ridge, MFs, and CCs, the data suggest a one order of magnitude decrease toward the ionization front at the optical bar. The highest angular resolution (12 arcsec) map in the J = 24-23 line shows this emission to be strongly concentrated around the BN/KL region. Its spatial distribution exhibits an incomplete ringlike structure with IRc2 at the inner edge. It is suggested that the HC3N ring constitutes the wall of the cavity where the slow-wind from IRc2 is plunging.

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