Structure and chemistry of Orion S

Details Structure and chemistry of Orion S Structure and chemistry of Orion S

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...405..599m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 405, no. 2, p. 599-607.

Astronomy and Astrophysics

Astrophysics

30

Abundance, Early Stars, Emission Spectra, Interstellar Chemistry, Orion Nebula, Radio Spectra, Star Formation, Density (Mass/Volume), Depletion, Formyl Ions, Gas Flow, Hydrocyanic Acid, Methyl Alcohol, Millimeter Waves, Shock Wave Interaction, Silicon Dioxide, Silicon Oxides

Scientific paper

We present interferometric observations of the SiO J = 2-1, H13CO(+) J = 1-0, HC3N J = 11-10, CH3OH J(K) = 2(0)-1(0), and SO2 J(KpK0) = 8(17)-8(08) transitions along with the 3.1 mm continuum toward the young stellar object Orion S. The HC3N and H13CO(+) emission trace similar spatial and velocity distributions which are extended and follow the Orion molecular ridge. The SiO emission is more spatially confined, peaking to the west of the 3.1 mm continuum source, while the CH3OH emission peaks to the southwest. Weak SO2 emission was detected southeast of the continuum source position. Column densities and fractional abundances are derived for each species at different positions in the region. In general, the molecular abundances near the continuum source are similar to those in the quiescent material near IRc 2, but the abundances decrease toward the continuum source position indicating localized depletions of at least a factor of three. The presence of strong SiO emission with much weaker SO2 emission is interpreted as resulting from high-velocity shock interactions between the outflow from Orion S and the surrounding cloud.

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