H II Regions and Photodissociation Regions in NGC 6334

Details H II Regions and Photodissociation Regions in NGC 6334 H II Regions and Photodissociation Regions in NGC 6334

Dec 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...189.2105j&link_type=abstract

American Astronomical Society, 189th AAS Meeting, #21.05; Bulletin of the American Astronomical Society, Vol. 28, p.1303

Astronomy and Astrophysics

Astronomy

Scientific paper

We present new VLA 3 cm continuum images of the southern portion of the H II region/molecular cloud complex NGC 6334. The radio continuum source G351.20+0.70, first discovered by Moran et al. (1990), is resolved into a 1 pc (2') diameter shell. In addition, we have discovered an unresolved radio counterpart to the near IR source NGC 6334 A-IRS 20, as well as three unresolved radio sources coincident with the FIR source NGC 6334 V. The G351.20+0.70 radio shell is surrounded by [C II] 158 um emission, which in turn is surrounded by CO emission. Apparently, it is a classical photodissociation region, although the ionizing source or sources remain unidentified. A B0 ZAMS star is required to account for the observed radio flux. The unresolved radio sources associated with IRS 20 and NGC 6334 V are consistent with Stromgren spheres surrounding B2 ZAMS stars in a region of fairly high electron density (n ~ 50,000 cm(-3) ). The inferred stellar luminosity, however, cannot account for the observed infrared luminosity. A cluster of lower mass stars may account for this discrepancy. Alternatively, the stars may be in a protostellar phase and derive most of their luminosity from accretion.

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