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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Final published version
Research output: Contribution to Journal/Magazine › Journal article › peer-review
| <mark>Journal publication date</mark> | 11/10/2016 |
|---|---|
| <mark>Journal</mark> | Monthly Notices of the Royal Astronomical Society |
| Issue number | 1 |
| Volume | 462 |
| Number of pages | 9 |
| Pages (from-to) | 181-189 |
| Publication Status | Published |
| Early online date | 11/07/16 |
| <mark>Original language</mark> | English |
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.