We use cookies to ensure that we give you the best experience on our website. By continuing to browse this repository, you give consent for essential cookies to be used. You can read more about our Privacy and Cookie Policy.

Durham Research Online
You are in:

The evolution of gas-phase metallicity and resolved abundances in star-forming galaxies at z ≍ 0.6-1.8

Gillman, S. and Tiley, A.L. and Swinbank, A.M. and Dudzevičiūtė, U. and Sharples, R.M. and Smail, Ian and Harrison, C.M. and Bunker, Andrew J. and Bureau, Martin and Cirasuolo, M. and Magdis, Georgios E. and Mendel, Trevor and Stott, John P. (2021) 'The evolution of gas-phase metallicity and resolved abundances in star-forming galaxies at z ≍ 0.6-1.8.', Monthly notices of the Royal Astronomical Society, 500 (3). pp. 4229-4247.


We present an analysis of the chemical abundance properties of ≈650 star-forming galaxies at z ≈ 0.6–1.8. Using integral-field observations from the K-band multi-object spectrograph (KMOS), we quantify the [N II]/H α emission-line ratio, a proxy for the gas-phase oxygen abundance within the interstellar medium. We define the stellar mass–metallicity relation at z ≈ 0.6–1.0 and z ≈ 1.2–1.8 and analyse the correlation between the scatter in the relation and fundamental galaxy properties (e.g. H α star formation rate, H α specific star formation rate, rotation dominance, stellar continuum half-light radius, and Hubble-type morphology). We find that for a given stellar mass, more highly star-forming, larger, and irregular galaxies have lower gas-phase metallicities, which may be attributable to their lower surface mass densities and the higher gas fractions of irregular systems. We measure the radial dependence of gas-phase metallicity in the galaxies, establishing a median, beam smearing corrected, metallicity gradient of ΔZ/ΔR = 0.002 ± 0.004 dex kpc−1, indicating on average there is no significant dependence on radius. The metallicity gradient of a galaxy is independent of its rest-frame optical morphology, whilst correlating with its stellar mass and specific star formation rate, in agreement with an inside–out model of galaxy evolution, as well as its rotation dominance. We quantify the evolution of metallicity gradients, comparing the distribution of ΔZ/ΔR in our sample with numerical simulations and observations at z ≈ 0–3. Galaxies in our sample exhibit flatter metallicity gradients than local star-forming galaxies, in agreement with numerical models in which stellar feedback plays a crucial role redistributing metals.

Item Type:Article
Full text:(VoR) Version of Record
Download PDF
Publisher Web site:
Publisher statement:This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2020 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Date accepted:28 October 2020
Date deposited:29 June 2021
Date of first online publication:31 October 2020
Date first made open access:29 June 2021

Save or Share this output

Look up in GoogleScholar