Ammonia observations of G34.3 + 0.1 - A 'bipolar' H II region?

Details Ammonia observations of G34.3 + 0.1 - A 'bipolar' H II region? Ammonia observations of G34.3 + 0.1 - A 'bipolar' H II region?

Nov 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985mnras.217..485h&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 217, Nov. 15, 1985, p. 485-492.

Astronomy and Astrophysics

Astronomy

30

Ammonia, Astronomical Spectroscopy, Density Distribution, H Ii Regions, Line Spectra, Milky Way Galaxy, Molecular Clouds, Spectral Resolution

Scientific paper

G34.3 + 0.1 has been mapped in the (1,1) and (2,2) inversion line transitions of ammonia with 2.2 arcmin resolution using the 25-m radio telescope at Chilbolton, Hampshire, and with 40 arcsec resolution using the 100-m Effelsberg telescope. The observations delineate a molecular cloud with a central core and a total mass of approximately several thousand solar masses. The 'cometary' appearance of one of its associated H II regions is probably best explained by the presence of density gradients within the molecular cloud and not, as has been suggested by Reid and Ho, by the effects of a stellar wind from the precursor to the supernova remnant W44. A detailed comparison of the LSR velocities of the ambient cloud, the OH masers, and recombination line emission from the H II region suggests that the OH masers may be part of a central turbulent disc confining a bipolar outflow. They are not part of a remnant cloud collapsing on to a recently formed H II region as proposed by Garay et al.

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