The evolution of dust in the local and high-redshift universe

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https://www.cambridge.org/core/journals/proceedings-of-the-international-astronomical-union/article/evolution-of-dust-in-the-local-and-highredshift-universe/C1DEC66141A14933F36223F8756A9514

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https://doi.org/10.1017/S1743921316004804
 http://hdl.handle.net/11603/24858

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UMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)
UMBC Faculty Collection

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https://orcid.org/0000-0001-8403-8548
 https://orcid.org/0000-0001-7380-3144

Date

2016-10-27

Type of Work

conference papers and preoceedings
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Citation of Original Publication

Dwek, E., Arendt, R., Staguhn, J., & Temim, T. (2015). The evolution of dust in the local and high-redshift universe. Proceedings of the International Astronomical Union, 11(A29B), 182-183. doi:10.1017/S1743921316004804

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This is a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law.
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Abstract

Dust is a ubiquities component of the interstellar medium (ISM) of galaxies, and manifests itself in many different ways. Yet, its origin, composition, and size distribution are still a matter of great debate. Most of the thermally condensed dust is produced in the explosively expelled ejecta of core collapse supernovae (CCSNe) and in the quiescent winds of AGB stars. Following its injection into the ISM it is destroyed by supernova (SN) shock waves. Knowing the relative rates of these processes is crucial for understanding the nature and evolution of dust in galaxies. In the following we will review three aspects of the evolution of dust in galaxies: the evolution of dust in the ejecta of SN1987A; the rates of dust production and destruction rates in the Magellanic Clouds (MCs), and the evolution of dust in CLASH 2882, a gravitationally-lensed galaxy at z=1.