Hostname: page-component-586b7cd67f-gb8f7 Total loading time: 0 Render date: 2024-11-22T23:30:52.786Z Has data issue: false hasContentIssue false
  • English
  • Français

The relation between dust amount and galaxy mass across the cosmic time

Published online by Cambridge University Press:  29 March 2021

J. H. Barbosa-Santos Open the ORCID record for J. H. Barbosa-Santos [Opens in a new window]  and
G. B. Lima Neto
J. H. Barbosa-Santos
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosférica, USP, Rua do Matão, 1226 - Cidade Universitária, 05508-090, São Paulo, SP, Brazil email: [email protected]
G. B. Lima Neto
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosférica, USP, Rua do Matão, 1226 - Cidade Universitária, 05508-090, São Paulo, SP, Brazil email: [email protected]
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 Obscured Galaxies (DOGs) are observed as far as the reionization epoch. Their cosmic density peaks together with the star formation rate. DOGs also rule the star formation in high stellar mass galaxies. In this work we used a chemodynamical model to evolve the amount of dust in galaxies. We ran forty models varying initial mass and both dust formation efficiency and dust production. We find that for high star formation rate systems the accretion dominates the dust evolution and it explains high-z DOGs. Low star formation rate systems are better suited to investigate dust production. Also, we find that a MDust/MGas versus MDust/M* diagram is a good tracer of galaxy evolution.

Keywords

galaxies: evolutiongalaxies: ISMgalaxies: high-redshift(ISM:) dustextinction
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S359: Galaxy Evolution and Feedback across Different Environments , March 2019 , pp. 342 - 344
Copyright
© The Author(s), 2021. Published by Cambridge University Press on behalf of International Astronomical Union

References

Barbosa-Santos, J. H., Lima Neto, G. B., & Friaça, A. C. S. 2020, MNRAS submitted Google Scholar
Dwek, E. 1998, ApJ, 501, 643 CrossRefGoogle Scholar
Friaça, A. C. S. & Barbuy, B. 2017 A&A, 598, A121 CrossRefGoogle Scholar
Friaça, A. C. S. & Terlevich, R. J. 1998 MNRAS, 298, 399 CrossRefGoogle Scholar
Gioannini, L., Matteucci, F., Vladilo, G., et al. 2017 MNRAS, 464, 985 CrossRefGoogle Scholar
Knudsen, K. K., Watson, D., Frayer, D., et al. 2017 MNRAS, 466, 138 CrossRefGoogle Scholar
Lianou, S., Xilouris, E., Madden, S. C., et al. 2016 MNRAS, 461, 2856 CrossRefGoogle Scholar
Magdis, G. F., Rigopoulou, D., Daddi, E., et al. 2017, A&A, 603, A93 Google Scholar
Rémy-Ruyer, A., Madden, S. C., Galliano, F., et al. 2014, A&A, 563, A31 Google Scholar
Rémy-Ruyer, A., Madden, S. C., Galliano, F., et al. 2015, A&A, 582, A121 Google Scholar
Whitaker, K. E., Pope, A., Cybulski, R., et al. 2017 ApJ, 850, 208 CrossRefGoogle Scholar