Hostname: page-component-cd9895bd7-dzt6s Total loading time: 0 Render date: 2024-12-23T18:56:45.953Z Has data issue: false hasContentIssue false
  • English
  • Français

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

Published online by Cambridge University Press:  27 October 2016

Eli Dwek ,
Richard G. Arendt ,
Johannes Staguhn  and
Tea Temim
Eli Dwek
Affiliation:
NASA at Goddard Space Flight Center, Observational Cosmology Lab., Greenbelt, MD 20771, USA, e-mail: [email protected]
Richard G. Arendt
Affiliation:
NASA at Goddard Space Flight Center, Observational Cosmology Lab., Greenbelt, MD 20771, USA, e-mail: [email protected] CRESST, University of Maryland, Baltimore County Baltimore, MD 21250, USA
Johannes Staguhn
Affiliation:
NASA at Goddard Space Flight Center, Observational Cosmology Lab., Greenbelt, MD 20771, USA, e-mail: [email protected] The Henry A. Rowland Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA
Tea Temim
Affiliation:
NASA at Goddard Space Flight Center, Observational Cosmology Lab., Greenbelt, MD 20771, USA, e-mail: [email protected] CRESST, University of Maryland-College Park, College Park, MD 20742, USA
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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.

Keywords

DustsupernovaeSN1987AMagellanic CloudsgalaxiesCLASH 2882
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29B: Astronomy in Focus , August 2015 , pp. 182 - 183
Copyright
Copyright © International Astronomical Union 2016 

References

Dwek, E. & Arendt, R. G. 2015, ApJ, 810, 75 CrossRefGoogle Scholar
Dwek, E., Staguhn, J., Arendt, R. G. et al. 2015, ApJ, in pressGoogle Scholar
Temim, T., Dwek, E., Tchernyshyov, K., et al. 2015, ApJ, 799, 158 Google Scholar
Matsuura, M., Dwek, E., Barlow, M. J., et al. 2015, ApJ, 800, 50 CrossRefGoogle Scholar