SiO in Barnard 1

Details SiO in Barnard 1 SiO in Barnard 1

Aug 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992pasj...44..459y&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 44, no. 4, p. 459-467.

Astronomy and Astrophysics

Astronomy

15

Emission Spectra, Interstellar Matter, Silicon Oxides, Star Formation, Abundance, Electron Transitions, Ground State, Infrared Sources (Astronomy), Molecular Flow, Vibrational Spectra

Scientific paper

The emission lines of the J = 2-1 and J = 1-0 transitions of SiO in the vibrational ground state were observed toward a low-mass-star-forming region, Barnard 1 (B1), with the Nobeyama 45-m radiotelescope. The distribution of the J = 2-1 line of SiO was investigated using the Nobeyama Millimeter Array with a spatial resolution of 8 x 10 arcsec. At least two compact clumps of SiO were found near the IRAS source position. These two clumps have both blueshifted and redshifted velocity components, suggesting that they were possibly formed by an interaction between the molecular outflow and the dense gas around a newly born protostar. On the basis of LVG statistical equilibrium calculations, the fractional abundance of SiO in B1 was estimated to be (0.9-1.7) x 10 exp -8. This value is by three orders of magnitude larger than the upper limit to the fractional abundance in the cold dark cloud (TMC1).

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