Galaxy metallicity scaling relations in the EAGLE simulations
We quantify the correlations between gas-phase and stellar metallicities and global properties of galaxies, such as stellarmass, halomass, age and gas fraction, in the Evolution and Assembly of GaLaxies and their Environments suite of cosmological hydrodynamical simulations. The slope of the correla...
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| Acceso en línea: | http://hdl.handle.net/20.500.12110/paper_00358711_v472_n3_p3354_DeRossi |
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todo:paper_00358711_v472_n3_p3354_DeRossi2023-10-03T14:47:22Z Galaxy metallicity scaling relations in the EAGLE simulations De Rossi, M.E. Bower, R.G. Font, A.S. Schaye, J. Theuns, T. Cosmology: theory Galaxies: abundances Galaxies: evolution Galaxies: haloes Galaxies: highredshift Galaxies: star formation We quantify the correlations between gas-phase and stellar metallicities and global properties of galaxies, such as stellarmass, halomass, age and gas fraction, in the Evolution and Assembly of GaLaxies and their Environments suite of cosmological hydrodynamical simulations. The slope of the correlation between stellar mass and metallicity of star-forming (SF) gas (M*- ZSF,gas relation) depends somewhat on resolution, with the higher resolution run reproducing a steeper slope. This simulation predicts a non-zero metallicity evolution, increasing by ≈0.5 dex at ~109M⊙ since z = 3. The simulated relation between stellar mass, metallicity and star formation rate at z ≲ 5 agrees remarkably well with the observed fundamental metallicity relation. At M* ≲ 1010.3 M⊙ and fixed stellar mass, higher metallicities are associated with lower specific star formation rates, lower gas fractions and older stellar populations. On the other hand, at higher M*, there is a hint of an inversion of the dependence of metallicity on these parameters. The fundamental parameter that best correlates with the metal content, in the simulations, is the gas fraction. The simulated gas fraction-metallicity relation exhibits small scatter and does not evolve significantly since z = 3. In order to better understand the origin of these correlations, we analyse a set of lower resolution simulations in which feedback parameters are varied. We find that the slope of the simulated M*-ZSF,gas relation is mostly determined by stellar feedback at low stellar masses (M* ≲ 1010 M⊙), and at high masses (M* ≳ 1010 M⊙) by the feedback from active galactic nuclei. © 2017 The Authors. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00358711_v472_n3_p3354_DeRossi |
| institution |
Universidad de Buenos Aires |
| institution_str |
I-28 |
| repository_str |
R-134 |
| collection |
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
| topic |
Cosmology: theory Galaxies: abundances Galaxies: evolution Galaxies: haloes Galaxies: highredshift Galaxies: star formation |
| spellingShingle |
Cosmology: theory Galaxies: abundances Galaxies: evolution Galaxies: haloes Galaxies: highredshift Galaxies: star formation De Rossi, M.E. Bower, R.G. Font, A.S. Schaye, J. Theuns, T. Galaxy metallicity scaling relations in the EAGLE simulations |
| topic_facet |
Cosmology: theory Galaxies: abundances Galaxies: evolution Galaxies: haloes Galaxies: highredshift Galaxies: star formation |
| description |
We quantify the correlations between gas-phase and stellar metallicities and global properties of galaxies, such as stellarmass, halomass, age and gas fraction, in the Evolution and Assembly of GaLaxies and their Environments suite of cosmological hydrodynamical simulations. The slope of the correlation between stellar mass and metallicity of star-forming (SF) gas (M*- ZSF,gas relation) depends somewhat on resolution, with the higher resolution run reproducing a steeper slope. This simulation predicts a non-zero metallicity evolution, increasing by ≈0.5 dex at ~109M⊙ since z = 3. The simulated relation between stellar mass, metallicity and star formation rate at z ≲ 5 agrees remarkably well with the observed fundamental metallicity relation. At M* ≲ 1010.3 M⊙ and fixed stellar mass, higher metallicities are associated with lower specific star formation rates, lower gas fractions and older stellar populations. On the other hand, at higher M*, there is a hint of an inversion of the dependence of metallicity on these parameters. The fundamental parameter that best correlates with the metal content, in the simulations, is the gas fraction. The simulated gas fraction-metallicity relation exhibits small scatter and does not evolve significantly since z = 3. In order to better understand the origin of these correlations, we analyse a set of lower resolution simulations in which feedback parameters are varied. We find that the slope of the simulated M*-ZSF,gas relation is mostly determined by stellar feedback at low stellar masses (M* ≲ 1010 M⊙), and at high masses (M* ≳ 1010 M⊙) by the feedback from active galactic nuclei. © 2017 The Authors. |
| format |
JOUR |
| author |
De Rossi, M.E. Bower, R.G. Font, A.S. Schaye, J. Theuns, T. |
| author_facet |
De Rossi, M.E. Bower, R.G. Font, A.S. Schaye, J. Theuns, T. |
| author_sort |
De Rossi, M.E. |
| title |
Galaxy metallicity scaling relations in the EAGLE simulations |
| title_short |
Galaxy metallicity scaling relations in the EAGLE simulations |
| title_full |
Galaxy metallicity scaling relations in the EAGLE simulations |
| title_fullStr |
Galaxy metallicity scaling relations in the EAGLE simulations |
| title_full_unstemmed |
Galaxy metallicity scaling relations in the EAGLE simulations |
| title_sort |
galaxy metallicity scaling relations in the eagle simulations |
| url |
http://hdl.handle.net/20.500.12110/paper_00358711_v472_n3_p3354_DeRossi |
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AT derossime galaxymetallicityscalingrelationsintheeaglesimulations AT bowerrg galaxymetallicityscalingrelationsintheeaglesimulations AT fontas galaxymetallicityscalingrelationsintheeaglesimulations AT schayej galaxymetallicityscalingrelationsintheeaglesimulations AT theunst galaxymetallicityscalingrelationsintheeaglesimulations |
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1782026015690719232 |