Examining Interstellar Dust from X-rays to Infrared

Details Examining Interstellar Dust from X-rays to Infrared Examining Interstellar Dust from X-rays to Infrared

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.0169v&link_type=abstract

American Astronomical Society, HEAD meeting #9, #1.69; Bulletin of the American Astronomical Society, Vol. 38, p.340

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Scientific paper

While interstellar dust is vitally important to the Galaxy, being necessary both in stellar system and molecule formation, the grains' exact nature remains mysterious. Although their effects are seen in almost all astronomical observations, where they both scatter and absorb light in the sightline, they are very difficult to study. Dust grain models, which are necessary for the recovery of an object's spectral energy distribution and a comprehensive understanding of dust grains, rely on data from the UV through IR regimes and elemental abundances for constraints; however, numerous models meet these conditions and there is no way to distinguish among them. Thus, data from other regimes are needed to impose tighter constraints. X-ray dust halos provide an excellent, and mostly untapped, diagnostic of grain characteristics and can allow us to discriminate among grain models. We have obtained data covering the broadest wavelength regime ever considered in dust studies -- XMM-Newton imagery plus UV through IR data -- for the sightline toward the high mass X-ray binary X Persei. These will be applied to leading dust models, finally allowing us to discriminate amongst them and develop a more complete understanding of the nature of dust grains.

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