Skip to main content

Research Repository

Advanced Search

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

Gillman, S.; Tiley, A.L.; Swinbank, A.M.; Dudzevičiūtė, U.; Sharples, R.M.; Smail, Ian; Harrison, C.M.; Bunker, Andrew J.; Bureau, Martin; Cirasuolo, M.; Magdis, Georgios E.; Mendel, Trevor; Stott, John P.

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


Authors

S. Gillman

A.L. Tiley

C.M. Harrison

Andrew J. Bunker

Martin Bureau

M. Cirasuolo

Georgios E. Magdis

Trevor Mendel

John P. Stott



Abstract

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.

Journal Article Type Article
Acceptance Date Oct 28, 2020
Online Publication Date Oct 31, 2020
Publication Date 2021-01
Deposit Date May 5, 2021
Publicly Available Date Jun 29, 2021
Journal Monthly Notices of the Royal Astronomical Society
Print ISSN 0035-8711
Electronic ISSN 1365-2966
Publisher Royal Astronomical Society
Peer Reviewed Peer Reviewed
Volume 500
Issue 3
Pages 4229-4247
DOI https://doi.org/10.1093/mnras/staa3400
Public URL https://durham-repository.worktribe.com/output/1248607
Publisher URL https://ui.adsabs.harvard.edu/abs/2021MNRAS.500.4229G

Files

Published Journal Article (9.3 Mb)
PDF

Copyright 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.






You might also like



Downloadable Citations