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The nature of Hbeta+[O III] and [O II] emitters to z ˜ 5 with HiZELS: stellar mass functions and the evolution of EWs
Khostovan, A. A.; Sobral, D.; Mobasher, B.; Smail, I.; Darvish, B.; Nayyeri, H.; Hemmati, S.; Stott, J. P.
AA(Department of Physics & Astronomy, University of California, Riverside, CA 92512, USA ), AB(Department of Physics, Lancaster University, Lancaster LA1 4YB, UK; Leiden Observatory, Leiden University, PO Box 9513, NL-2300 RA Leiden, the Netherlands), AC(Department of Physics & Astronomy, University of California, Riverside, CA 92512, USA), AD(Centre for Extragalactic Astrophysics, Department of Physics, Durham University, Durham DH1 3LE, UK; Institute for Computational Cosmology, Durham University, Durham DH1 3LE, UK), AE(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA), AF(Department of Physics & Astronomy, University of California, Irvine, CA 92697, USA), AG(Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA), AH(Subdepartment of Astrophysics, Department of Physics, University of Oxford, Oxford OX1 3RH, UK)
Monthly Notices of the Royal Astronomical Society, Volume 463, Issue 3, p.2363-2382 (MNRAS Homepage)
Publication Date:
Astronomy Keywords:
galaxies: evolution, galaxies: fundamental parameters, galaxies: high-redshift, galaxies: star formation, cosmology: observations
Abstract Copyright:
2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
Bibliographic Code:


We investigate the properties of ˜7000 narrow-band selected galaxies with strong Hbeta+[O III] and [O II] nebular emission lines from the High-z Emission-Line Survey between z ˜ 0.8 and 5.0. Our sample covers a wide range in stellar mass (Mstellar ˜ 107.5-12.0 M&sun;), rest-frame equivalent widths (EWrest˜10-105 Å), and line luminosities (Lline ˜ 1040.5-43.2 erg s-1). We measure the Hbeta+[O III]-selected stellar mass functions out to z ˜ 3.5 and find that both M* and phi* increases with cosmic time. The [O II]-selected stellar mass functions show a constant M* ≈ 1011.6 M&sun; and a strong, increasing evolution with cosmic time in phi* in line with Halpha studies. We also investigate the evolution of the EWrest as a function of redshift with a fixed mass range (109.5-10.0 M&sun;) and find an increasing trend best represented by (1 + z)3.81 ± 0.14 and (1 + z)2.72 ± 0.19 up to z ˜ 2 and ˜3 for Hbeta+[O III] and [O II] emitters, respectively. This is the first time that the EWrest evolution has been directly measured for Hbeta+[O III] and [O II] emitters up to these redshifts. There is evidence for a slower evolution for z > 2 in the Hbeta+[O III] EWrest and a decreasing trend for z > 3 in the [O II] EWrest evolution, which would imply low [O II] EW at the highest redshifts and higher [O III]/[O II] line ratios. This suggests that the ionization parameter at higher redshift may be significantly higher than the local Universe. Our results set the stage for future near-IR space-based spectroscopic surveys to test our extrapolated predictions and also produce z > 5 measurements to constrain the high-z end of the EWrest and [O III]/[O II] evolution.
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