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Modeling dust in a universe of galaxies

Published online by Cambridge University Press:  04 June 2020

Desika Narayanan Open the ORCID record for Desika Narayanan [Opens in a new window] ,
Qi Li ,
Romeel Davé ,
Charlie Conroy ,
Benjamin D. Johnson  and
Gergo Popping
Desika Narayanan
Affiliation:
Department of Astronomy, University of Florida, 211 Bryant Space Sciences Center, Gainesville, FL, 32611, USA email: desika.narayanan@ufl.edu University of Florida Informatics Institute, 432 Newell Drive, CISE Bldg E251, Gainesville, FL, 32611, USA Cosmic Dawn Centre, Niels Bohr Institute, University of Copenhagen and DTU-Space, Technical University of Denmark
Qi Li
Affiliation:
Department of Astronomy, University of Florida, 211 Bryant Space Sciences Center, Gainesville, FL, 32611, USA email: desika.narayanan@ufl.edu
Romeel Davé
Affiliation:
Institute for Astronomy, Royal Observatory, University of Edinburgh, Edinburgh, EH9 3HJ, UK University of the Western Cape, Bellville, Cape Town, 7535, South Africa South African Astronomical Observatories, Observatory, Cape Town, 7925, South Africa
Charlie Conroy
Affiliation:
Department of Astronomy, Harvard University, 60 Garden Street, Cambridge, MA, 02138, USA
Benjamin D. Johnson
Affiliation:
Department of Astronomy, Harvard University, 60 Garden Street, Cambridge, MA, 02138, USA
Gergo Popping
Affiliation:
European Southern Observatory, Karl-Schartzchild-Strasse 2, 85748, Garching, Germany
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Abstract

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In this invited talk, we discuss the physics of the lifecycle of dust in the context of galaxy formation simulations. After outlining the basic physical processes, we apply algorithms for the formation, growth, and destruction of dust in the ISM to a state-of-the-art cosmological simulation to develop a model for the evolution of the dust to gas and dust to metals ratios in galaxies. We show that while modern simulations are able to match the observed dust mass function at redshift z = 0, most models underpredict the observed mass function at high-redshift (z = 2). We then show the power of these techniques by expanding our model to include a spectrum of dust sizes, and make initial predictions for extinction laws in local galaxies.

Keywords

ISM: dustextinctiongalaxies: ISMgalaxies: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S352: Uncovering Early Galaxy Evolution in the ALMA and JWST Era , June 2019 , pp. 44 - 54
Copyright
© International Astronomical Union 2020

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