Mapping the Outflow of OH:5.89-0.39

Details Mapping the Outflow of OH:5.89-0.39 Mapping the Outflow of OH:5.89-0.39

Sep 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.246..217z&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 246, NO.2/SEP15, P. 217, 1990

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Scientific paper

A fast, massive bipolar outflow is found to be associated with 5.89-0.39, a luminous, compact H II region. Using VLA observations, we have mapped the source in the continuum, in several OH lines, in H I absorption, and in the H76α recombination line.
The inner ionized region, with a radius of 0.06 pc, shows a disc-like geometry, with some evidence for rotation in the outer part of the disc. The main-line OH masers in the surrounding neutral gas trace a biconical rapid outflow, with a total velocity width of 60 km s-1, perpendicular to the disc. The OH outflow is aligned with a much more extended flow observed in CO. Evidence for outflow is also seen in H I absorption, albeit at lower velocities. We conclude that the outflowing gas originates outside the ionized region. The H2O masers also trace an outflow, but with a velocity gradient opposite to the OH and CO. They may arise from one or more other young stars in the region.
The distance, derived from H I absorption, is about 4 kpc; the luminosity is a few times 105 Lsun. The central star is most likely a massive star of late O-type, still surrounded by an accretion disc left over from the star-formation process.
5.89-0.39 is among the most massive and luminous, and contains the most luminous H II region, of the known outflow objects. The characteristics of the OH emission differ from other outflow sources: in 5.89-0.39 the OH is situated in the outflowing gas, while in other known cases it is either aligned with the disc, or shows a chaotic velocity field. This makes 5.89-0.39 very suitable for studying the dynamics of massive molecular outflows. We suggest that the OH emitting clumps arise from a disrupting circumstellar disc.

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