@article{2d1bcdb0cf814a6e8965d2448140d46b,
title = "[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",
abstract = "We investigate the properties of z = 2.23 Ha and [O III] λ5007 emitters using the narrow-bandselected 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 Ha and/or [O III] emission lines, most of the sources detected with both Ha 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 [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 Ha emission is no longer observable from the ground.",
keywords = "Galaxies: evolution, Galaxies: high-redshift",
author = "Suzuki, {T. L.} and T. Kodama and D. Sobral and Khostovan, {A. A.} and M. Hayashi and R. Shimakawa and Y. Koyama and Tadaki, {K. I.} and I. Tanaka and Y. Minowa and M. Yamamoto and I. Smail and Best, {P. N.}",
note = "Funding Information: We thank the anonymous referee for careful reading and comments that improved the clarity of this paper. TLS acknowledges to Professor Lisa Kewley for kindly accepting the visit to Mt. Stromlo Observatory for 3 months. The major part of this paper was written during the stay. TLS is also grateful to her group members for the many ways in which they helped. TK acknowledges the financial support in part by a Grant-in-Aid for the Scientific Research (Nos 21340045 and 24244015) by the Japanese Ministry of Education, Culture, Sports and Science. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship, from FCT through a FCT Investigator Starting Grant and Startup Grant (IF/01154/2012/CP0189/CT0010), and from FCT grant PEst-OE/FIS/UI2751/2014. IS acknowledges support from STFC (ST/L00075X/1), theERCAdvanced GrantDUSTYGAL(321334), and a Royal Society/Wolfson Merit Award. PNB is grateful for support from the UK STFC via grant ST/M001229/1. Publisher Copyright: {\textcopyright} 2016 The Authors.",
year = "2016",
month = oct,
day = "11",
doi = "10.1093/mnras/stw1655",
language = "English",
volume = "462",
pages = "181--189",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "1",
}