The evolution of galaxy metallicity scaling relations in cosmological hydrodynamical simulations

Rossi, M. E. De; Theuns, Tom; Font, Andreea S.; McCarthy, Ian G.

doi:10.1093/mnras/stv1287

Cited by 36 publications

(34 citation statements)

References 99 publications

(191 reference statements)

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“…At a given M * , the metallicity of low-mass systems decreases with SFR while, for massive galaxies, the metallicity increases with SFR. Similar trends were reported by Yates et al (2012) and De Rossi et al (2015b) in the context of semi-analytical models and hydrodynamical simulations, respectively. Lagos et al (2016) explored the relation between SF gas metallicity, SFR and M * in the EAGLE Ref-L100N1504 simulation.…”

Section: F U N Da M E N Ta L M E Ta L L I C I T Y R E L At I O N a N supporting

confidence: 85%

“…It is clear that the scatter in the data at z ≈ 0 is larger than predicted by simulations (see also Schaye et al 2015). This was also noted by De Rossi et al (2015b) when using the GIMIC simulations and might be related to uncertainties in observed stellar metallicity determinations. Gallazzi et al (2005) adopted a Bayesian statistical approach to obtain Z * for individual galaxies, estimating the 68 per cent confidence interval within which this parameter is constrained.…”

Section: The M * -Z * R E L At I O Nmentioning

confidence: 56%

“…Bothwell et al 2013;Hughes et al 2013). De Rossi et al (2015b) obtained that dependence in the case of GIMIC galaxies while Lagos et al (2016) found similar results by performing a principal component analysis over different galaxy properties in the EAGLE Ref-L100N1504 simulation. At a given M * , galaxies with higher gas fractions tend to exhibit higher SFRs and, as we have discussed, these galaxies have lower gas-phase metallicities.…”

Section: F U N Da M E N Ta L M E Ta L L I C I T Y R E L At I O N a N mentioning

confidence: 64%

“…However, intermediate-resolution simulations run in different volumes show similar metallicity relations, suggesting a weak influence of environment on the obtained trends. By analysing GIMIC simulations, De Rossi et al (2015b) also found that metallicity scaling relations are not significantly affected by the large-scale environment. Recent observations suggest a small dependence of the MZR on the environment (e.g.…”

Section: 1mentioning

confidence: 92%

“…In addition, the GIMIC simulations do not reproduce the observed flattening of the MZR at the high-mass end. De Rossi et al (2015b) claimed that the latter issue is probably related to the lack of active galactic nucleus (AGN) feedback in GIMIC.…”

Section: Introductionmentioning

confidence: 99%

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Galaxy metallicity scaling relations in the EAGLE simulations

Rossi

Bower

Font

et al. 2017

Monthly Notices of the Royal Astronomical Society

138

136

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Citation for published item:he ossiD w r¡ % imili nd fowerD i h rd qF nd pontD endree F nd h yeD toop nd heunsD om @PHIUA 9q l xy met lli ity s ling rel tions in the ieqvi simul tionsF9D wonthly noti es of the oy l estronomi l o ietyFD RUP @QAF ppF QQSREQQUUF Further information on publisher's website: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTWe quantify the correlations between gas-phase and stellar metallicities and global properties of galaxies, such as stellar mass, halo mass, 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 * -Z SF,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 ∼10 9 M 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 * 10 10.3 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 * -Z SF,gas relation is mostly determined by stellar feedback at low stellar masses (M * 10 10 M ), and at high masses (M * 10 10 M ) by the feedback from active galactic nuclei.

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Section: F U N Da M E N Ta L M E Ta L L I C I T Y R E L At I O N a N supporting

confidence: 85%

Section: The M * -Z * R E L At I O Nmentioning

confidence: 56%

Section: F U N Da M E N Ta L M E Ta L L I C I T Y R E L At I O N a N mentioning

confidence: 64%

Section: 1mentioning

confidence: 92%

Section: Introductionmentioning

confidence: 99%

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Galaxy metallicity scaling relations in the EAGLE simulations

Rossi

Bower

Font

et al. 2017

Monthly Notices of the Royal Astronomical Society

138

136

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Gas Accretion and Galactic Chemical Evolution: Theory and Observations

Finlator

2017

Gas Accretion Onto Galaxies

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This chapter reviews how galactic inflows influence galaxy metallicity. The goal is to discuss predictions from theoretical models, but particular emphasis is placed on the insights that result from using models to interpret observations. Even as the classical "G-dwarf problem" endures in the latest round of observational confirmation, a rich and tantalizing new phenomenology of relationships between M * , Z, SFR, and gas fraction is emerging both in observations and in theoretical models. A consensus interpretation is emerging in which star-forming galaxies do most of their growing in a quiescent way that balances gas inflows and gas processing, and metal dilution with enrichment. Models that explicitly invoke this idea via equilibrium conditions can be used to infer inflow rates from observations, while models that do not assume equilibrium growth tend to recover it self-consistently. Mergers are an overall subdominant mechanism for delivering fresh gas to galaxies, but they trigger radial flows of previously-accreted gas that flatten radial gas-phase metallicity gradients and temporarily suppress central metallicities. Radial gradients are generically expected to be steep at early times and then flattened by mergers and enriched inflows of recycled gas at late times. However, further theoretical work is required in order to understand how to interpret observations. Likewise, more observational work is needed in order to understand how metallicity gradients evolve to high redshifts.

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Gas Accretion and Star Formation Rates

Alméida

2017

Gas Accretion Onto Galaxies

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Cosmological numerical simulations of galaxy evolution show that accretion of metal-poor gas from the cosmic web drives the star formation in galaxy disks. Unfortunately, the observational support for this theoretical prediction is still indirect, and modeling and analysis are required to identify hints as actual signs of star-formation feeding from metal-poor gas accretion. Thus, a meticulous interpretation of the observations is crucial, and this observational review begins with a simple theoretical description of the physical process and the key ingredients it involves, including the properties of the accreted gas and of the star-formation that it induces. A number of observations pointing out the connection between metalpoor gas accretion and star-formation are analyzed, specifically, the short gas consumption time-scale compared to the age of the stellar populations, the fundamental metallicity relationship, the relationship between disk morphology and gas metallicity, the existence of metallicity drops in starbursts of star-forming galaxies, the socalled G dwarf problem, the existence of a minimum metallicity for the star-forming gas in the local universe, the origin of the α-enhanced gas forming stars in the local universe, the metallicity of the quiescent BCDs, and the direct measurements of gas accretion onto galaxies. A final section discusses intrinsic difficulties to obtain direct observational evidence, and points out alternative observational pathways to further consolidate the current ideas.

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The evolution of galaxy metallicity scaling relations in cosmological hydrodynamical simulations

Cited by 36 publications

References 99 publications

Galaxy metallicity scaling relations in the EAGLE simulations

Galaxy metallicity scaling relations in the EAGLE simulations

Gas Accretion and Galactic Chemical Evolution: Theory and Observations

Gas Accretion and Star Formation Rates

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