Recycled stellar ejecta as fuel for star formation and implications for the origin of the galaxy mass–metallicity relation

Segers, Marijke C.; Crain, Robert A.; Schaye, Joop; Bower, Richard G.; Furlong, Michelle; Schaller, Matthieu; Theuns, Tom

doi:10.1093/mnras/stv2562

Cited by 46 publications

(60 citation statements)

References 87 publications

(120 reference statements)

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“…Our results regarding the increasing metallicity of the SF gas with time are consistent with Segers et al (2016a), who show that recycling of stellar mass-loss in EAGLE becomes increasingly important for fuelling star formation towards lower redshift. Also, Segers et al (2016a) determined a characteristic mass, M * ≈ 10 10.5 M , below which, the contribution of recycled mass increases with mass and above which, it decreases with mass.…”

Section: Evolution Of the M * -Z Sfgas Relationsupporting

confidence: 91%

“…2 and the flattening of the slope of the z = 0 MZR at high masses ( Fig. 1) might reflect the transition determined by Segers et al (2016a). These authors claimed that this transition reflects the transition from stellar to AGN feedback.…”

Section: Evolution Of the M * -Z Sfgas Relationmentioning

confidence: 66%

“…Columns list: simulations identifiers, the side length of the volume (L) and the particle number per species (i.e. gas, DM) per dimension (N), the power-law slope of the polytropic equation of state of SF gas (γ eos ), the power-law index of the star formation law (n), the asymptotic maximum (f th,max ) and minimum (f th,min ) values of f th (equation 3), the parameters that control the characteristic density and the power-law slope of the density dependence of the energy feedback from star formation (n H,0 and n n , respectively), the subgrid accretion disc viscosity parameter (C visc model in EAGLE yields a better description of the global metal enrichment of massive galaxies, generating the observed turn-over of the MZR at the high-mass end, as was also shown by Segers et al (2016a). The plan of the paper is as follows.…”

Section: Introductionmentioning

confidence: 71%

“…Also, Segers et al (2016a) determined a characteristic mass, M * ≈ 10 10.5 M , below which, the contribution of recycled mass increases with mass and above which, it decreases with mass. The negligible evolution that we obtained for the M * = 10 10.5 -10 11.0 M bin in Fig.…”

Section: Evolution Of the M * -Z Sfgas Relationmentioning

confidence: 94%

“…(ii) The flattening of the slope of the simulated M * -O/H| SF,gas relation at the high-mass end is mainly the result of AGN feedback (see also Segers et al 2016a). To explore the role of AGN feedback, we used intermediate-resolution simulations as we needed to focus on the trends at high masses.…”

Section: O N C L U S I O N Smentioning

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

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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: Evolution Of the M * -Z Sfgas Relationsupporting

confidence: 91%

Section: Evolution Of the M * -Z Sfgas Relationmentioning

confidence: 66%

Section: Introductionmentioning

confidence: 71%

Section: Evolution Of the M * -Z Sfgas Relationmentioning

confidence: 94%

Section: O N C L U S I O N Smentioning

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

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141

136

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The Effect of Galactic Feedback on Gas Accretion and Wind Recycling

Voort

2017

Gas Accretion Onto Galaxies

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In the absence of galactic winds, the rate at which gas accretes onto galaxies is determined by the gravitational potential and by radiative cooling. However, outflows driven by supernovae and active galactic nuclei not only eject gas from galaxies, but also prevent gas from accreting in the first place. Furthermore, gas previously ejected from a galaxy can re-accrete onto (the same or a different) galaxy. Because this gas has a high metallicity, its cooling rate is relatively high, which will increase its chances to re-accrete. This complex interplay between gas inflows and outflows is discussed in this chapter. Wind recycling is found to be an important process that fuels galaxies at late times and the recycled gas has different properties than gas accreting for the first time. Quantitative conclusions, however, vary between studies, because the amount of wind recycling is dependent on the details of the feedback model. We discuss these differences, known caveats, and ways to make progress in understanding how galaxies are fed at low redshift.

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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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Recycled stellar ejecta as fuel for star formation and implications for the origin of the galaxy mass–metallicity relation

Cited by 46 publications

References 87 publications

Galaxy metallicity scaling relations in the EAGLE simulations

Galaxy metallicity scaling relations in the EAGLE simulations

The Effect of Galactic Feedback on Gas Accretion and Wind Recycling

Gas Accretion and Star Formation Rates

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