SMC-Type Interstellar Dust in the Milky Way

Abstract

It is well known that the sightline toward HD 204827 in the cluster Trumpler 37 shows an UV extinction curve that does not follow CCM. However, when a dust component, foreground to the cluster, is removed, the residual extinction curve is identical to that found in the SMC within the uncertainties. The curve is very steep and has little or no 2175 A bump. The position of HD 204827 in the sky is projected onto the edge of the Cepheus IRAS Bubble. In addition, HD 204827 has an IRAS bowshock indicating that it may be embedded in dust swept up by the supernova that created the IRAS Bubble. Shocks due to the supernova may have led to substantial processing of this dust. The HD 204827 cloud is dense and rich in carbon molecules. The 3.4 $\mu$m feature indicating a C-H grain mantle is present in the dust toward HD 204827. The environment of the HD 204827 cloud dust may be similar to the dust associated with HD 62542 which lies on the edge of a stellar wind bubble and is also dense and rich in molecules. This sightline may be a Rosetta Stone if its environment can be related to those in the SMC having similar dust.

18 pages, 5 figures, ApJ in press

References in corpus (2)

• A Quantitative Comparison of SMC, LMC, and Milky Way UV to NIR Extinction Curves
• A Method of Correcting Near-Infrared Spectra for Telluric Absorption

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