The 22 micron emission feature in supernova remnants and massive star-forming regions

Details The 22 micron emission feature in supernova remnants and massive star-forming regions The 22 micron emission feature in supernova remnants and massive star-forming regions

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009eimw.confe..11o&link_type=abstract

"The Evolving ISM in the Milky Way and Nearby Galaxies, The Fourth Spitzer Science Center Conference, Proceedings of the confere

Physics

Dust, Extinction, Supernovae: General, Supernova Remnant, Hii Regions

Scientific paper

Spitzer/IRS observations have confirmed the presence of the broad emission feature around 22 μm in the Carina nebula suggested by ISO/SWS observations. They have indicated that the feature peak is located around 23 μm and the band width/profile may vary in the nebula. It has been suggested that the feature originates from dust grains formed in supernovae since a similar feature has also been reported in Cas A SNR. IRS observations of Cas A confirm the feature, but it seems to peak at a little shorter wavelength (about 21 μm) and has a sharper profile than that seen in the Carina nebula. IRS spectra of some HII regions also show a broad emission feature similar to the Carina spectrum. These results suggest that dust grains relating to SNe or massive star-formation have a feature around 20--23 μm, which may originate from dust grains with similar optical characteristics. We suggest that the shape effect of surface modes of FeO grains could account for the observed variety of the features if the shape distribution evolves from a nearly mono-shape (spherical shape) distribution to a continuous shape distribution possibly by coagulation. The understanding of the nature of the feature is important for the investigation of recent star-formation activities in external galaxies.

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