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Title:
A fundamental metallicity relation for galaxies at z = 0.84-1.47 from HiZELS
Authors:
Stott, John P.; Sobral, David; Bower, Richard; Smail, Ian; Best, Philip N.; Matsuda, Yuichi; Hayashi, Masao; Geach, James E.; Kodama, Tadayuki
Affiliation:
AA(Institute for Computational Cosmology, Durham University, South Road, Durham DH1 3LE, UK; ), AB(Leiden Observatory, Leiden University, PO Box 9513, NL-2300 RA Leiden, the Netherlands), AC(Institute for Computational Cosmology, Durham University, South Road, Durham DH1 3LE, UK), AD(Institute for Computational Cosmology, Durham University, South Road, Durham DH1 3LE, UK), AE(SUPA, Institute for Astronomy, Royal Observatory of Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK), AF(National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; The Graduate University for Advanced Studies (SOKENDAI), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan), AG(Institute for Cosmic Ray Research, The University of Tokyo, Kashiwa 277-8582, Japan), AH(Centre for Astrophysics Research, Science & Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB, UK), AI(National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Subaru Telescope, National Astronomical Observatory of Japan, 650 North Aohoku Place, Hilo, HI 96720, USA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 436, Issue 2, p.1130-1141 (MNRAS Homepage)
Publication Date:
12/2013
Origin:
OUP
Astronomy Keywords:
galaxies: abundances, galaxies: evolution, galaxies: star formation
Abstract Copyright:
2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
DOI:
10.1093/mnras/stt1641
Bibliographic Code:
2013MNRAS.436.1130S

Abstract

We obtained Subaru FMOS observations of Halpha emitting galaxies selected from the HiZELS, to investigate the relationship between stellar mass, metallicity and star formation rate (SFR) at z = 0.84-1.47, for comparison with the fundamental metallicity relation seen at low redshift. Our findings demonstrate, for the first time with a homogeneously selected sample, that a relationship exists for typical star-forming galaxies at z ˜ 1-1.5 and that it is surprisingly similar to that seen locally. Therefore, star-forming galaxies at z ˜ 1-1.5 are no less metal abundant than galaxies of similar mass and SFR at z ˜ 0.1, contrary to claims from some earlier studies. We conclude that the bulk of the metal enrichment for this star-forming galaxy population takes place in the 4 Gyr before z ˜ 1.5. We fit a new mass-metallicity-SFR plane to our data which is consistent with other high-redshift studies. However, there is some evidence that the mass-metallicity component of this high-redshift plane is flattened, at all SFR, compared with z ˜ 0.1, suggesting that processes such as star formation-driven winds, thought to remove enriched gas from low-mass haloes, are yet to have as large an impact at this early epoch. The negative slope of the SFR-metallicity relation from this new plane is consistent with the picture that the elevation in the SFR of typical galaxies at z ≳ 1 is fuelled by the inflow of metal-poor gas and not major merging.
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