Effective yields as tracers of feedback effects on metallicity scaling relations in the EAGLE cosmological simulations

Author:

Zerbo M C123ORCID,De Rossi M E23ORCID,Lara-López M A45ORCID,Cora S A16ORCID,Zenocratti L J16ORCID

Affiliation:

1. Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, B1900FWA La Plata , Argentina

2. Universidad de Buenos Aires, Facultad de Ciencias Exactas y Naturales, C1428EGA Buenos Aires , Argentina

3. CONICET – Universidad de Buenos Aires, Instituto de Astronomía y Física del Espacio (IAFE), C1428ZAA Buenos Aires , Argentina

4. Departamento de Física de la Tierra y Astrofísica, Universidad Complutense de Madrid , E-28040 Madrid , Spain

5. Instituto de Física de Partículas y del Cosmos IPARCOS, Facultad de Ciencias Físicas, Universidad Complutense de Madrid , E-28040 Madrid , Spain

6. Instituto de Astrofísica de La Plata, CONICET – Universidad Nacional de La Plata , Paseo del Bosque s/n, B1900FWA La Plata , Argentina

Abstract

ABSTRACT Effective yields, yeff, are defined by fundamental galaxy properties (i.e. stellar mass M⋆, gas mass Mgas, and gas-phase metallicity). For a closed-box model, yeff is constant and equivalent to the mass in metals returned to the gas per unit mass locked in long-lived stars. Deviations from such behaviour have been often considered observational signatures of past feedback events. By analysing eagle simulations with different feedback models, we evaluate the impact of supernovae (SNe) and active galactic nuclei (AGNs) feedback on yeff at redshift z = 0. When removing supermassive black holes (BHs) and, hence, AGN effects, in simulations, galaxies are located around a plane in the M⋆–Mgas–O/H parameter space (being O/H a proxy for gas metallicity, as usual), with such a plane roughly describing a surface of constant yeff. As the ratio between BH mass and M⋆ increases, galaxies deviate from that plane towards lower yeff as a consequence of AGN feedback. For galaxies not strongly affected by AGN feedback, a stronger SN feedback efficiency generates deviations towards lower yeff, while galaxies move towards the opposite side of the plane (i.e. towards higher values of yeff) as SN feedback becomes weaker. Star-forming galaxies observed in the Local Universe are located around a similar 3D plane. Our results suggest that the features of the scatter around the observed plane are related to the different feedback histories of galaxies, which might be traced by yeff.

Funder

CONICET

Universidad Nacional de La Plata

STFC

Durham University

Publisher

Oxford University Press (OUP)

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