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

Suzuki, T.L. and Kodama, T. and Sobral, D. and Khostovan, A.A. and Hayashi, M. and Shimakawa, R. and Koyama, Y. and Tadaki, K.-i. and Tanaka, I. and Minowa, Y. and Yamamoto, M. and Smail, I. and Best, P.N. (2016) '[O III] emission line as a tracer of star-forming galaxies at high redshifts : comparison between Hα and [O III] emitters at z=2.23 in HiZELS.', Monthly notices of the Royal Astronomical Society., 462 (1). pp. 181-189.


We investigate the properties of z = 2.23 Hα and [O III] λ5007 emitters using the narrow-band-selected samples obtained from the High-z Emission Line Survey. We construct two samples of the Hα and [O III] emitters and compare their integrated physical properties. We find that the distribution of stellar masses, dust extinction, star formation rates (SFRs), and specific SFRs (sSFRs) 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 [O III] emission lines, most of the sources detected with both Hα and [O III] show log(sSFRUV) ≳ −9.5. The comparison of the three subsamples suggests that sources with strong [O III] line emission tend to have the highest star-forming activity out all galaxies that we study. We argue that the [O III] 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.

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Publisher statement:This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Date accepted:07 July 2016
Date deposited:10 November 2016
Date of first online publication:11 July 2016
Date first made open access:10 November 2016

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