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Oxygen abundances of zCOSMOS galaxies at z ∼ 1.4 based on five lines and implications for the fundamental metallicity relation

Published online by Cambridge University Press:  09 February 2015

Christian Maier ,
Simon J. Lilly ,
Bodo L. Ziegler  and
zCOSMOS team
Christian Maier
Affiliation:
Department for Astrophysics, University of Vienna, Türkenschanzstr. 17, 1180 Vienna, Austria email: christian.maier@univie.ac.at
Simon J. Lilly
Affiliation:
Institute of Astronomy, ETH Zurich, 8093 Zurich, Switzerland
Bodo L. Ziegler
Affiliation:
Department for Astrophysics, University of Vienna, Türkenschanzstr. 17, 1180 Vienna, Austria email: christian.maier@univie.ac.at
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Abstract

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A relation between the stellar mass M and the gas-phase metallicity Z of galaxies, the MZR, is observed up to higher redshifts. It is a matter of debate, however, if the SFR is a second parameter in the MZR. To explore this issue at z > 1, we used VLT-SINFONI near-infrared (NIR) spectroscopy of eight zCOSMOS galaxies at 1.3 < z < 1.4 to measure the strengths of four emission lines: Hβ, [OIII]λ5007, Hα, and [NII]λ6584, additional to [OII]λ3727 measured from VIMOS. We derive reliable O/H metallicities based on five lines, and also SFRs from extinction corrected Hα measurements. We find that the MZR of these star-forming galaxies at z ≈ 1.4 is lower than the local SDSS MZR by a factor of three to five, a larger change than reported in the literature using [NII]/Hα-based metallicities from individual and stacked spectra. Correcting N2-based O/Hs using recent results by Newman et al. (2014), also the larger FMOS sample at z ∼ 1.4 of Zahid et al. (2014) shows a similar evolution of the MZR like the zCOSMOS objects. These observations seem also in agreement with a non-evolving FMR using the physically motivated formulation of the FMR from Lilly et al. (2013).

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S309: Galaxies in 3D across the Universe , July 2014 , pp. 281 - 282
Copyright
Copyright © International Astronomical Union 2015 

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