Correlations between mass, stellar kinematics and gas metallicity in EAGLE galaxies

Abstract

The metallicity of star-forming gas in galaxies from the EAGLE simulations increases with stellar mass. Here we investigate whether the scatter around this relation correlates with morphology and/or stellar kinematics. At redshift $z=0$, galaxies with more rotational support have lower metallicities on average when the stellar mass is below $M_{\star }\approx 10^{10}{\mathrm{M}}_{\odot }$. This trend inverts at higher values of $M_{\star }$, when prolate galaxies show typically lower metallicity. At increasing redshifts, the trend between rotational support and metallicity becomes weaker at low stellar mass but more pronounced at high stellar mass. We argue that the secondary dependence of metallicity on stellar kinematics is another manifestation of the observed anti-correlation between metallicity and star formation rate at a given stellar mass. At low masses, such trends seem to be driven by the different star-formation histories of galaxies and stellar feedback. At high masses, feedback from active galactic nuclei and galaxy mergers play a dominant role.

arXiv comment5 pages, 4 figures. Accepted for publication in MNRAS

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• Galaxy And Mass Assembly (GAMA): The inferred mass--metallicity relation from z=0 to 3.5 via forensic SED fitting
• Explaining the scatter in the galaxy mass-metallicity relation with gas flows
• Diagnosing the interstellar medium of galaxies with far-infrared emission lines II. [C II], [O I], [O III], [N II] and [N III] up to z=6
• The origin of correlations between mass, metallicity and morphology in galaxies from the EAGLE simulation