Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 421, Issue 1, Pages 486-501Publisher
OXFORD UNIV PRESS
DOI: 10.1111/j.1365-2966.2011.20327.x
Keywords
dust, extinction; H II regions; galaxies: abundances; galaxies: ISM
Categories
Funding
- NSFC [10973013, 11073017, 11033007]
- 973 Program [2009CB824800]
- Fundamental Research Funds for the Central Universities
- Alfred P. Sloan Foundation
- National Science Foundation
- US Department of Energy
- National Aeronautics and Space Administration
- Japanese Monbukagakusho
- Max Planck Society
- Higher Education Funding Council for England
- American Museum of Natural History
- Astrophysical Institute Potsdam
- University of Basel
- University of Cambridge
- Case Western Reserve University
- University of Chicago
- Drexel University
- Fermilab
- Institute for Advanced Study
- Japan Participation Group
- Johns Hopkins University
- Joint Institute for Nuclear Astrophysics
- Kavli Institute for Particle Astrophysics and Cosmology
- Korean Scientist Group
- Chinese Academy of Sciences (LAMOST)
- Los Alamos National Laboratory
- Max Planck Institute for Astronomy (MPIA)
- Max Planck Institute for Astrophysics (MPA)
- New Mexico State University
- Ohio State University
- University of Pittsburgh
- University of Portsmouth
- Princeton University
- United States Naval Observatory
- University of Washington
Ask authors/readers for more resources
We present empirical relations between the global dust reddening and other physical galaxy properties including the Ha luminosity, Ha surface brightness, metallicity and axial ratio for star-forming disc galaxies. The study is based on a large sample of similar to 22 000 well-defined star-forming galaxies selected from the Sloan Digital Sky Survey. The reddening parametrized by colour excess E(B - V) is derived from the Balmer decrement. Besides the dependency of reddening on Ha luminosity/surface brightness and gas phase metallicity, it is also correlated with the galaxy inclination, in the sense that edge-on galaxies are more attenuated than face-on galaxies at a given intrinsic luminosity. In light of these correlations, we present the empirical formulae of E(B - V) as a function of these galaxy properties, with a scatter of only 0.07 mag. The empirical relations can be reproduced if most dust attenuation to the H II region is due to diffuse interstellar dust distribution in a disc thicker than that of the H II region. The empirical formulae can be incorporated into semi-analytical models of galaxy formation and evolution to estimate the dust reddening and more practically enable comparison with observations.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available