Probing the Grains Responsible for Extinction Using Small Magellanic Cloud Sightlines

Details Probing the Grains Responsible for Extinction Using Small Magellanic Cloud Sightlines Probing the Grains Responsible for Extinction Using Small Magellanic Cloud Sightlines

Jul 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002hst..prop.9383g&link_type=abstract

HST Proposal ID #9383

Computer Science

Hst Proposal Id #9383

Scientific paper

Small Magellanic Cloud sightlines have the greatest potential to relate specific interstellar extinction features to distinct grain properties. The reasons for this are 1} prominent extinction features such as the 2175 Angstrom bump and the far-ultraviolet rise vary among SMC targets and 2} grain types may be very different from those in the Galaxy. Specifically, Welty et al. {2001} recently identified an SMC sightline that contains dust, but no silicate grains. Silicates are a dominant source of extinction in all dust models; the SMC may be the only location where the importance of silicates can be verified or disproven. We propose to explore the relationship between grain types and extinction toward 2 SMC stars with very different extinction curves; AzV 18 lacks a 2175 Angstrom bump and has a strong far-UV rise while the extinction curve towards the SMC star AzV 456 has a prominent 2175 Angstrom bump and a much weaker far-UV rise. We will compare the interstellar abundances of atoms that are prevalent in silicates {Si, Mg, Fe} toward these 2 stars and use the results to constrain dust extinction models. These SMC observations, which can only be obtained with STIS, are the only direct way to probe the connection between grain types/environments and extinction. The results from this study will be useful for modeling and understanding all regions that contain dust {AGN, circumstellar disks, star formation regions, etc.}.

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