Physical Properties of the Giant H II Region G353.2+0.9 in NGC 6357

Details Physical Properties of the Giant H II Region G353.2+0.9 in NGC 6357 Physical Properties of the Giant H II Region G353.2+0.9 in NGC 6357

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004jkas...37..281b&link_type=abstract

Journal of the Korean Astronomical Society, vol. 37, no. 4, pp. 281-284

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Ism: H Ii Regions, Ism:Individual (Ngc 6357)

Scientific paper

Optical imaging and spectroscopy of G353.2+0.9, the brightest part of the giant H II region NGC 6357, shows that this H II region is optically thin, contains ˜ 300 M&sun; of ionized gas and is probably expanding into the surrounding medium. Its chemical composition is similar to that found in other H II regions at similar galactocentric distances if temperature fluctuations are significant. The inner regions are probably made of thin shells and filaments, whereas extended slabs of material, maybe shells seen edge-on, are found in the periphery. The radio continuum and Hα emission maps are very similar, indicating that most of the optical nebula is not embedded in the denser regions traced by molecular gas and the presence of IR sources. About 1050 UV photons per second are required to produce the Hβ flux from the 11.3'x10' region surrounding the Pis 24 cluster that is south of G353.2+0.9. Most of the energy powering this region is produced by the O3-7 stars in Pis 24. Most of the 2MASS sources in the field with large infrared excesses are within G353.2+0.9, indicating that the most recent star forming process occured within it. The formation of Pis 24 preceded and caused the formation of this new generation of stars and may be responsible for the present-day morphology of the entire NGC 6357 region.

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