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  • 1607.02054v1

    Rights statement: This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record is available online at: http://mnras.oxfordjournals.org/content/462/1/181.abstract

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[OIII] emission line as a tracer of star-forming galaxies at high redshifts: comparison between Hα and [OIII] emitters at z=2.23 in HiZELS

Research output: Contribution to journalJournal article

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  • T. L. Suzuki
  • T. Kodama
  • D. Sobral
  • A. A. Khostovan
  • M. Hayashi
  • R. Shimakawa
  • Y. Koyama
  • K. -i. Tadaki
  • I. Tanaka
  • Y. Minowa
  • M. Yamamoto
  • I. Smail
  • P. N. Best
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<mark>Journal publication date</mark>11/10/2016
<mark>Journal</mark>Monthly Notices of the Royal Astronomical Society
Issue number1
Volume462
Number of pages9
Pages (from-to)181-189
Publication statusPublished
Early online date11/07/16
Original languageEnglish

Abstract

We investigate the properties of z=2.23 Hα and [Oiii]λ5007 emitters using the narrow-bandselected samples obtained from the High-z Emission Line Survey (HiZELS: Sobral et al. 2013). We construct two samples of the Hα and [Oiii] emitters and compare their integrated physical properties. We find that the distribution of stellar masses, dust extinction, star formation rates (SFRs), and specific SFRs, is not statistically different between the two samples. When we separate the full galaxy sample into three subsamples according to the detections of the Hα and/or [Oiii] emission lines, most of the sources detected with both Hα and [Oiii] show log(sSFRUV)&-9.5. The comparison of the three subsamples suggests that sources with strong [Oiii] line emission tend to have the highest star-forming activity out all galaxies that we study. We argue that the [Oiii] emission line can be used as a tracer of star-forming galaxies at high redshift, and that it is especially useful to investigate star-forming galaxies at z>3, for which Hα emission is no longer observable from the ground.

Bibliographic note

This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record is available online at: http://mnras.oxfordjournals.org/content/462/1/181.abstract