Mufasa: Galaxy star formation, gas, and metal properties across cosmic time

Davé, Romeel; Rafieferantsoa, Mika; Thompson, Raymond H.; Hopkins, Philip F.

doi:10.1093/mnras/stx108

Cited by 176 publications

(255 citation statements)

References 126 publications

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“…There, we show that the implementation of energy feedback from star formation that depends on the local density and metallicity leads to an evolution of the MZR consistent with the observed trend (see e.g. Fu et al 2012 andDavé et al 2017, for similar findings derived from other models and simulations). On the other hand, a constant energy feedback, as that implemented in GIMIC, leads to a negligible MZR evolution.…”

Section: Evolution Of the M * -Z Sfgas Relationsupporting

confidence: 86%

Galaxy metallicity scaling relations in the EAGLE simulations

Rossi

Bower

Font

et al. 2017

Monthly Notices of the Royal Astronomical Society

144

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: Evolution Of the M * -Z Sfgas Relationsupporting

confidence: 86%

Galaxy metallicity scaling relations in the EAGLE simulations

Rossi

Bower

Font

et al. 2017

Monthly Notices of the Royal Astronomical Society

144

136

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“…However, at z > 0 the normalization is lower than what most observations indicate, a tension that is in common to all large-volume cosmological hydrodynamical simulations (e.g. Furlong et al 2015;Davé et al 2017).…”

Section: Discussionmentioning

confidence: 79%

The size evolution of star-forming and quenched galaxies in the IllustrisTNG simulation

Genel

Nelson

Pillepich

et al. 2017

Monthly Notices of the Royal Astronomical Society

298

240

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We analyze scaling relations and evolution histories of galaxy sizes in TNG100, part of the IllustrisTNG simulation suite. Observational qualitative trends of size with stellar mass, starformation rate and redshift are reproduced, and a quantitative comparison of projected r-band sizes at 0 z 2 shows agreement to much better than 0.25 dex. We follow populations of z = 0 galaxies with a range of masses backwards in time along their main progenitor branches, distinguishing between main-sequence and quenched galaxies. Our main findings are as follows. (i) At M * ,z=0 10 9.5 M , the evolution of the median main progenitor differs, with quenched galaxies hardly growing in median size before quenching, whereas main-sequence galaxies grow their median size continuously, thus opening a gap from the progenitors of quenched galaxies. This is partly because the main-sequence high-redshift progenitors of quenched z = 0 galaxies are drawn from the lower end of the size distribution of the overall population of main-sequence high-redshift galaxies. (ii) Quenched galaxies with M * ,z=0 10 9.5 M experience a steep size growth on the size-mass plane after their quenching time, but with the exception of galaxies with M * ,z=010 11 M , the size growth after quenching is small in absolute terms, such that most of the size (and mass) growth of quenched galaxies (and its variation among them) occurs while they are still on the main-sequence. After they become quenched, the size growth rate of quenched galaxies as a function of time, as opposed to versus mass, is similar to that of main-sequence galaxies. Hence, the size gap is retained down to z = 0.

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“…These simulations utilize the suite of physics developed for the mufasa cosmological simulations as described in Davé et al (2016Davé et al ( , 2017. We refer the reader to these papers for more detail, and summarize the relevant details here.…”

Section: Cosmological Galaxy Formation Simulationsmentioning

confidence: 99%

SÍGAME Simulations of the , , and Line Emission from Star-forming Galaxies at

Olsen

Greve

Narayanan

et al. 2017

ApJ

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103

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Of the almost 40 star forming galaxies at z > ∼ 5 (not counting QSOs) observed in [C II] to date, nearly half are either very faint in [C II], or not detected at all, and fall well below expectations based on locally derived relations between star formation rate and [C II] luminosity. This has raised questions as to how reliable [C II] is as a tracer of star formation activity at these epochs and how factors such as metallicity might affect the [C II] emission. Combining cosmological zoom simulations of galaxies with SÍGAME (SImulator of GAlaxy Millimeter/submillimeter Emission) we have modeled the multi-phased interstellar medium ( We find that the [C II] emission is dominated by the diffuse ionized gas phase and molecular clouds, which on average contribute ∼ 66% and ∼ 27%, respectively. The molecular gas, which constitutes only ∼ 10% of the total gas mass is thus a more efficient emitter of [C II] than the ionized gas, which makes up ∼ 85% of the total gas mass. A principal component analysis shows that the [C II] luminosity correlates with the star formation activity of a galaxy as well as its average metallicity. The low metallicities of our simulations together with their low molecular gas mass fractions can account for their [C II]-faintness, and we suggest these factors may also be responsible for the [C II]-faint normal galaxies observed at these early epochs.

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Mufasa: Galaxy star formation, gas, and metal properties across cosmic time

Cited by 176 publications

References 126 publications

Galaxy metallicity scaling relations in the EAGLE simulations

Galaxy metallicity scaling relations in the EAGLE simulations

The size evolution of star-forming and quenched galaxies in the IllustrisTNG simulation

SÍGAME Simulations of the , , and Line Emission from Star-forming Galaxies at

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