Weak evolution of the mass–metallicity relation at cosmic dawn in the FirstLight simulations

Langan, Ivanna; Ceverino, Daniel; Finlator, Kristian

doi:10.1093/mnras/staa880

Cited by 30 publications

(38 citation statements)

References 42 publications

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“…This diversity in [OIII]/H𝛼 ratio depends primarily on the ionization parameter and secondarily on nebular metallicity (Figure 3). In our sample of low-metallicity galaxies, an increase in metallicity leads to higher line ratios, in a way similar to the [OIII]/H𝛽 ratio (Langan et al 2020). This is due to the low values of metallicity, log(Z/Z ) < −0.4, which place most of these galaxies in the ascending part of the [OIII]/H𝛽-Z curve (Gutkin et al 2016).…”

Section: Line Ratiossupporting

confidence: 63%

“…This range is partially due to the 1 dex variation in stellar mass of galaxies with similar UV luminosity (Ceverino et al 2019) and the factor 4 difference in SFR. Both the UV slope and the SFR-weighted, nebular metallicity (𝑍) exhibit a similar behaviour, driven by the diversity in stellar mass (Langan et al 2020) and SFR.…”

Section: Extreme Versus Typical Galaxiesmentioning

confidence: 89%

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FirstLight IV: Diversity in sub-L$_*$ galaxies at cosmic dawn

Ceverino,

Hirschmann,

Klessen

et al. 2021

Preprint

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Using a large sample of sub-L * galaxies, with similar UV magnitudes, M UV −19 at 𝑧 6, extracted from the FirstLight simulations, we show the diversity of galaxies at the end of the reionization epoch. We find a factor ∼40 variation in the specific star-formation rate (sSFR). This drives a ∼1 dex range in equivalent width of the [OIII]𝜆5007 line. Variations in nebular metallicity and ionization parameter within HII regions lead to a scatter in the equivalent widths and [OIII]/H𝛼 line ratio at a fixed sSFR. [OIII]-bright emitters have higher ionization parameters and/or higher metallicities than H𝛼-bright galaxies. According to the surface brightness maps in both [OIII] and H𝛼, [OIII]-bright emitters are more compact than H𝛼-bright galaxies. H𝛼 luminosity is higher than [OIII] if star formation is distributed over extended regions. OIII dominates if it is concentrated in compact clumps. In both cases, the H𝛼-emitting gas is significantly more extended than [OIII].

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Section: Line Ratiossupporting

confidence: 63%

Section: Extreme Versus Typical Galaxiesmentioning

confidence: 89%

FirstLight IV: Diversity in sub-L$_*$ galaxies at cosmic dawn

Ceverino,

Hirschmann,

Klessen

et al. 2021

Preprint

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“…Several groups have reported theoretical predictions for the MZR at high redshifts based on cosmological simulations. Bright z;8 galaxies near the mass range of our sample are predicted to have metallicities near ∼0.1 solar (Moriwaki et al 2018;Katz et al 2019;Langan et al 2020), with evolution in the MZR to z=8 of ∼0.5-0.9 dex (Figure 3; Ma et al 2016;Torrey et al 2019). These predictions are compatible and in fact in good agreement with our results.…”

Section: The Z;8 Mass-metallicity Relationmentioning

confidence: 83%

“…Both effects are expected to be prevalent given the sample's high SFRs. As an example, Langan et al (2020) report that gas flows reduce effective yields by a factor of 10 in simulated » z 8 galaxies. This drives the timescale to ∼100-300Myr to reach enrichment of ∼0.1 solar.…”

Section: Enrichment and Star Formation Timescalesmentioning

confidence: 99%

The Mass–Metallicity Relation at z ≃ 8: Direct-method Metallicity Constraints and Near-future Prospects

Jones

Roberts-Borsani

Ellis

et al. 2020

ApJ

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Physical properties of galaxies at z>7 are of interest for understanding both the early phases of star formation and the process of cosmic reionization. Chemical abundance measurements offer valuable information on the integrated star formation history, and hence ionizing photon production, as well as the rapid gas accretion expected at such high redshifts. We use reported measurements of [OIII]88 μm emission and star formation rate to estimate gasphase oxygen abundances in five galaxies at z=7.1-9.1 using the direct T e method. We find typical abundances + 12 log O H ( )=7.9 (∼0.2 times the solar value) and an evolution of 0.9±0.5 dex in oxygen abundance at fixed stellar mass from z;8 to 0. These results are compatible with theoretical predictions, albeit with large (conservative) uncertainties in both mass and metallicity. We assess both statistical and systematic uncertainties to identify promising means of improvement with the Atacama Large Millimeter/submillimeter Array (ALMA) and the James Webb Space Telescope (JWST). In particular we highlight [OIII]52 μm as a valuable feature for robust metallicity measurements. Precision of 0.1-0.2 dex in T e -based O/H abundance can be reasonably achieved for galaxies at z≈5-8 by combining [OIII]52 μm with rest-frame optical strong lines. It will also be possible to probe gas mixing and mergers via resolved T e -based abundances on kiloparsec scales. With ALMA and JWST, direct metallicity measurements will thus be remarkably accessible in the reionization epoch.

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“…The Z = 0.05 Z metallicity of SL2S 0217 is typical of z ∼ 6 galaxies with the same stellar mass (c.f. FIRSTLIGHT simulations, Langan et al 2020), underlining its suitability as a EoR analogue. Berg et al (2018, B18) and Erb et al (2019, E19), with the [C II] and CO(2-1) upper limits derived assuming the R ≤ 3 kpc aperture from the 1-arcsec taper images (Fig.…”

Section: Observations and Imagingmentioning

confidence: 99%

Ultra-faint [CII] emission in a redshift = 2 gravitationally-lensed metal-poor dwarf galaxy

Rybak,

da Cunha,

Groves

et al. 2021

Preprint

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Extreme emission-line galaxies (EELGs) at redshift z = 1 − 2 provide a unique view of metal-poor, starburst sources that are the likely drivers of the cosmic reionization at z ≥ 6. However, the molecular gas reservoirs of EELGs -the fuel for their intense star-formation -remain beyond the reach of current facilities. We present ALMA [C II] and PdBI CO(2-1) observations of a z = 1.8, strongly lensed EELG SL2S 0217, a bright Lymanα emitter with a metallicity 0.05 Z . We obtain a tentative (∼3-4σ) detection of the [C II] line and set an upper limit on the [C II]/SFR ratio of ≤ 1 × 10 6 L /(M yr −1 ), based on the synthesized images and visibilityplane analysis. The CO(2-1) emission is not detected. Photoionization modelling indicates that up to 80% of the [C II] emission originates from neutral or molecular gas, although we can not rule out that the gas is fully ionized. The very faint [C II] emission is in line with both nearby metal-poor dwarfs and high-redshift Lyman α emitters, and predictions from hydrodynamical simulations. However, the [C II] line is 30× fainter than predicted by the De Looze et al. ( 2014) [C II]-SFR relation for local dwarfs, illustrating the danger of extrapolating locally-calibrated relations to high-redshift, metal-poor galaxies.

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Weak evolution of the mass–metallicity relation at cosmic dawn in the FirstLight simulations

Cited by 30 publications

References 42 publications

FirstLight IV: Diversity in sub-L$_*$ galaxies at cosmic dawn

FirstLight IV: Diversity in sub-L$_*$ galaxies at cosmic dawn

The Mass–Metallicity Relation at z ≃ 8: Direct-method Metallicity Constraints and Near-future Prospects

Ultra-faint [CII] emission in a redshift = 2 gravitationally-lensed metal-poor dwarf galaxy

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