VLA spectral line observations of the H II complex G34.3+0.2

Details VLA spectral line observations of the H II complex G34.3+0.2 VLA spectral line observations of the H II complex G34.3+0.2

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...435..738f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 435, no. 2, p. 738-747

Astronomy and Astrophysics

Astronomy

22

Bow Waves, Fourier Analysis, Galactic Evolution, H Ii Regions, Radio Astronomy, Astronomical Maps, Astronomical Observatories, Emission Spectra, Flux Density, Photoionization

Scientific paper

Four H II regions have been previously detected toward the H II complex G34.3+0.2 in the radio continuum. Three of these regions (components A, B, and C) are ultracompact. The fourth, G34.3+0.2 component D, is an approximately equals 1 min (1.1 pc at 3.8 kpc) diameter ringlike H II region. We have observed the H93 alpha radio recombination line emission with approximately equals 11 sec spatial resolution and the 1.3 cm water maser emission with approximately equals 4 sec spatial resolution toward G34.3+0.2. The observed radio recombination line emission suggests that component D is an expanding shell source. The inferred expansion velocity of 5 km/s gives a calculated lifetime of approx. 105 yr. The continuum emission from the source is preferentially brightened on one side. We suggest that this asymmetric brightness distribution may be explained by the expansion of the H II region into an anisotropic medium. Alternatively, the increased brightness on the northwestern side could be the result of the superposition of two different H II regions. The average LSR velocity of the shell source has been determined to be 53.9 +/- 0.1 km/s. The observed spatial distribution of the H2O masers in the G34.3+0.2 complex has identified two new regions of star formation which are not associated with any radio continuum emission.

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