Variation of the nebular dust attenuation curve with the properties of local star-forming galaxies
Affiliation
Steward Observatory, University of ArizonaIssue Date
2021
Metadata
Show full item recordPublisher
Oxford University PressCitation
Rezaee, S., Reddy, N., Shivaei, I., Fetherolf, T., Emami, N., & Khostovan, A. A. (2021). Variation of the nebular dust attenuation curve with the properties of local star-forming galaxies. Monthly Notices of the Royal Astronomical Society, 506(3), 3588–3595.Rights
Copyright © 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
We use a sample of 78 340 star-forming galaxies at z ∼ 0.04-0.1 from the Sloan Digital Sky Survey (SDSS) data release (DR8) survey to calculate the average nebular dust attenuation curve and its variation with the physical properties of galaxies. Using the first four low-order Balmer emission lines (H α, H β, H γ, and H δ) detected in the composite spectrum of all galaxies in the sample, we derive a nebular attenuation curve in the range of 0.41 to 0.66, μm that has a similar shape and normalization to that of the Galactic extinction curve (Milky Way curve), the SMC curve and the nebular attenuation curve derived recently for typical star-forming galaxies at z ∼2. We divide the galaxies into bins of stellar mass, gas-phase metallicity, and specific star formation rate, and derive the nebular attenuation curve in each of these bins. This analysis indicates that there is very little variation in the shape of the nebular dust attenuation curve with the properties used to bin the galaxies, and suggests a near universal shape of the nebular dust attenuation curve at least among the galaxies and the range of properties considered in our sample. © 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.Note
Immediate accessISSN
0035-8711Version
Final published versionae974a485f413a2113503eed53cd6c53
10.1093/mnras/stab1885