High-resolution mapping of the bipolar outflow in NGC 2071 - Evidence for a wind-driven molecular outflow

Details High-resolution mapping of the bipolar outflow in NGC 2071 - Evidence for a wind-driven molecular outflow High-resolution mapping of the bipolar outflow in NGC 2071 - Evidence for a wind-driven molecular outflow

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...363..180k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 363, Nov. 1, 1990, p. 180-191.

Astronomy and Astrophysics

Astronomy

29

Astronomical Maps, Interstellar Matter, Molecular Flow, Nebulae, Stellar Winds, Carbon Disulfide, Carbon Monoxide, Line Spectra, Protostars, Radio Astronomy

Scientific paper

The bipolar outflow in NGC 2071 has been mapped in the CS (J = 2-1), CS (J = 1-0), HCO(+) (J = 1-0), and HCN (J = 1-0) lines, using the 45-m telescope of Nobeyama Radio Observatory with the narrow beams of HPBW = 20 arcsec and 40 arcsec. It is found that the rest components of the CS (J = 2-1) and CS (J = 1-0) lines have cavities at the centers of the red and blue lobes of the CO high-velocity emission, and that a single peak of the CS spectra outside the CO red lobe splits into two peaks inside the lobe. These features of the CS emission strongly suggest that the bipolar outflow in NGC 2071 consists of two expanding dense bubbles which are driven by a stellar wind from the IR cluster. The high-resolution mapping also reveals the fact that the CS bubbles have a clumpy structure. Two of the clumps are located at the place where the shocked H2 emission was detected. This fact indicates that formation of the strong shock results from the collision between the high-velocity wind from the IR cluster and the clumps in the ambient cloud. In addition, around the IR cluster this observation shows a disklike condensation, whose size is smaller than the width of the CO high-velocity outflow.

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