Hostname: page-component-54dcc4c588-xh45t Total loading time: 0 Render date: 2025-10-11T10:53:33.443Z Has data issue: false hasContentIssue false
  • English
  • Français

Dust reddening in star-forming galaxies

Published online by Cambridge University Press:  21 March 2013

Ting Xiao ,
Tinggui Wang ,
Huiyuan Wang ,
Hongyan Zhou ,
Honglin Lu  and
Xiaobo Dong
Ting Xiao*
Affiliation:
Partner Group of the Max Planck Institute for Astrophysics and Key Laboratory for Research in Galaxies and Cosmology of Chinese Academy of Sciences, Shanghai Astronomical Observatory, Nandan Road 80, Shanghai 200030, China
Tinggui Wang
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science & Technology of China, Hefei, Anhui 230026, China
Huiyuan Wang
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science & Technology of China, Hefei, Anhui 230026, China
Hongyan Zhou
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science & Technology of China, Hefei, Anhui 230026, China Polar Research Institute of China, Jinqiao Road 451, Shanghai 200136, China
Honglin Lu
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science & Technology of China, Hefei, Anhui 230026, China
Xiaobo Dong
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science & Technology of China, Hefei, Anhui 230026, China
*
†LAMOST fellow; Email: xiaoting@shao.ac.cn
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 crucial component of galaxies in modifying the observed properties of galaxies. Previous studies have suggested that dust reddening in star-forming galaxies is correlated with star formation rate (SFR), luminosity, gas-phase metallicity (Z), stellar mass (M*) and inclination. In this work we investigate the fundamental relations between dust reddening and physical properties of galaxies, and obtain a well-defined empirical recipe for dust reddening. The empirical formulae can be incorporated into semi-analytical models of galaxy formation and evolution to estimate the dust reddening and facilitate comparison with observations.

Keywords

galaxies: ISM — galaxies: abundances — HII regions — dustextinction

References

Kennicutt, R. C. Jr., 1998, ApJ, 498, 541CrossRefGoogle Scholar
Xiao, T., Wang, T.-G., Wang, H.-Y., Zhou, H.-Y., Lu, H.-L., & Dong, X.-B. 2012, MNRAS, 421, 486Google Scholar