Variation of the nebular dust attenuation curve with the properties of local star-forming galaxies

Saeed Rezaee, Naveen Reddy, Irene Shivaei, Tara Fetherolf, Najmeh Emami, A. A. Khostovan

Research output: Contribution to journalArticlepeer-review

1 Scopus citations

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.

Original languageEnglish (US)
Pages (from-to)3588-3595
Number of pages8
JournalMonthly Notices of the Royal Astronomical Society
Volume506
Issue number3
DOIs
StatePublished - Sep 1 2021

Bibliographical note

Publisher Copyright:
© 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.

Keywords

  • Dust, extinction
  • Galaxies: star formation
  • H ii regions
  • Local Group

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