Abstract
How dust absorbs and scatters starlight as a function of wavelength (known as the interstellar extinction curve) is crucial for correcting for the effects of dust extinction in inferring the true luminosity and colors of reddened astrophysical objects. Together with the extinction spectral features, the extinction curve contains important information about the dust size distribution and composition. This review summarizes our current knowledge of the dust extinction of the Milky Way, three Local Group galaxies (i.e., the Small and Large Magellanic Clouds, and M 31), and galaxies beyond the Local Group.
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Acknowledgements
We thank R.A. Benjamin, D.L. Block (DLB), G.C. Clayton, B.G. Elmegreen (BGE), B.T. Draine, G.G. Fazio, K.C. Freeman, M.L. Norman, M. Rubio, and A.N. Witt for helpful discussions. We are supported in part by NSFC 11373015 and 11173007, NSF AST-1109039, NASA NNX13AE63G, and the University of Missouri Research Board. It is a great pleasure to acknowledge the important role that DLB and BGE have played in pushing astrophysics to the new front. One of us (AL) would like to thank the SOC for inviting him to attend this fantastic, memorable conference in Seychelles.
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Li, A., Wang, S., Gao, J., Jiang, B. (2015). Dust in the Local Group. In: Freeman, K., Elmegreen, B., Block, D., Woolway, M. (eds) Lessons from the Local Group. Springer, Cham. https://doi.org/10.1007/978-3-319-10614-4_8
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