Simulations of High-redshift [O iii] Emitters: Chemical Evolution and Multiline Diagnostics

Nakazato, Yurina; Yoshida, Naoki; Ceverino, Daniel

doi:10.3847/1538-4357/ace25a

ApJ

2023

DOI: 10.3847/1538-4357/ace25a

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Simulations of High-redshift [O iii] Emitters: Chemical Evolution and Multiline Diagnostics

Yurina Nakazato

Naoki Yoshida

Daniel Ceverino

Abstract: Recent observations by the James Webb Space Telescope discovered a number of high-redshift galaxies with strong emission lines from doubly ionized oxygen. Combined with Atacama Large Millimeter/submillimeter Array observations of far-infrared lines, multiline diagnostics can be applied to the high-redshift galaxies in order to probe the physical conditions of the interstellar medium. We study the formation and evolution of galaxies using the FirstLight simulation suite, which provides outputs of 62 high-resolu… Show more

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Cited by 10 publications

References 80 publications

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Gas-phase metallicity gradients in galaxies at z ∼ 6–8

Venturi,

Carniani,

Parlanti

et al. 2024

A&A

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The study of gas-phase metallicity and its spatial distribution at high redshift is crucial to understand the processes that shaped the growth and evolution of galaxies in the early Universe. Here we study the spatially resolved metallicity in three systems at $z$ sim 6--8, namely and with JWST NIRSpec IFU low-resolution ($R$ sim 100) spectroscopic observations. These are among the highest-$z$ sources in which metallicity gradients have been probed so far. Each of these systems hosts several spatial components in the process of merging within a few kiloparsecs, identified from the rest-frame UV and optical stellar continuum and ionised gas emission line maps. The sources have heterogeneous properties, with stellar masses log($M_*/M_ sim 7.6--9.3, star formation rates (SFRs) sim 1--15 $M_ $, and gas-phase metallicities 12+log(O/H) sim 7.7--8.3, which exhibit a large scatter within each system. Their properties are generally consistent with those of the highest-redshift samples to date ($z$ sim 3--10), though the sources in and are at the high end of the mass-metallicity relation (MZR) defined by the $z$ sim 3--10 sources. Moreover, the targets in this work follow the predicted slope of the MZR at $z$ sim 6--8 from most cosmological simulations. The gas-phase metallicity gradients are consistent with being flat in the main sources of each system. Flat metallicity gradients are thought to arise from gas mixing processes on galaxy scales, such as mergers or galactic outflows and supernova winds driven by intense stellar feedback, which wash out any gradient formed in the galaxy. The existence of flat gradients at $z$ sim 6--8 sets also important constraints on future cosmological simulations and chemical evolution models, whose predictions on the cosmic evolution of metallicity gradients often differ significantly, especially at high redshift, but are mostly limited to z lesssim 3 so far.

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Gas-phase metallicity gradients in galaxies at z ∼ 6–8

Venturi,

Carniani,

Parlanti

et al. 2024

A&A

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show abstract

Constraining the physical properties of gas in high-z galaxies with far-infrared and submillimetre line ratios

Schimek,

Cicone,

Shen

et al. 2024

A&A

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Optical emission line diagnostics, which are a common tool for constraining the properties of the interstellar medium (ISM) of galaxies, become progressively inaccessible at higher redshifts for ground-based facilities. Far-infrared (FIR) emission lines, which are redshifted into atmospheric windows that are accessible for ground-based submillimetre facilities, could provide ISM diagnostics alternative to optical emission lines. We investigated FIR line ratios involving [CII] λ158 μm, [OIII] λ88 μm, [OIII] λ52 μm, [NII] λ122 μm, and [NIII] λ57 μm using synthetic emission lines applied to a high-resolution (mgas = 883.4 M⊙) cosmological zoom-in simulation, including radiative transfer post-processing with the code KRAMSES-RT at z = 6.5. We find that the [CII]/[NII]122 ratio is sensitive to the temperature and density of photodissociation regions. It might therefore be a useful tool for tracing the properties of this gas phase in galaxies. We also find that [NII]/[NIII] is a good tracer of the temperature and that [OIII]52/[OIII]88 is a good tracer of the gas density of HII regions. Emission line ratios containing the [OIII] λ88 μm line are sensitive to high-velocity outflowing gas.

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Redshift-dependent galaxy formation efficiency at z = 5 − 13 in the FirstLight Simulations

Ceverino,

Nakazato,

Yoshida

et al. 2024

A&A

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Some models of the formation of first galaxies predict low masses and faint objects at extremely high redshifts, $z However, the first observations of this epoch indicate a higher-than-expected number of bright (sometimes massive) galaxies. Numerical simulations can help to elucidate the mild evolution of the bright end of the UV luminosity function and they can provide the link between the evolution of bright galaxies and variations of the galaxy formation efficiency across different redshifts. We use the FirstLight database of 377 zoom-in cosmological simulations of a volume- and mass-complete sample of galaxies. Mock luminosities are estimated by a dust model constrained by observations of the beta -M$_ UV $ relation at $z=6-9$. FirstLight contains a high number of bright galaxies, M$_ UV -20$, consistent with current data at $z=6-13$. The evolution of the UV cosmic density is driven by the evolution of the galaxy efficiency and the relation between UV $ and halo mass. The efficiency of galaxy formation increases significantly with mass and redshift. At a fixed mass, galactic halos at extremely high redshifts convert gas into stars at a higher rate than at lower redshifts. The high gas densities in these galaxies enable high efficiencies. Our simulations predict higher number densities of massive galaxies, $ than other models with constant efficiency. Cosmological simulations of galaxy formation with detailed models of star formation and feedback can reproduce the different regimes of galaxy formation across cosmic history.

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Simulations of High-redshift [O iii] Emitters: Chemical Evolution and Multiline Diagnostics

Cited by 10 publications

References 80 publications

Gas-phase metallicity gradients in galaxies at z ∼ 6–8

Gas-phase metallicity gradients in galaxies at z ∼ 6–8

Constraining the physical properties of gas in high-z galaxies with far-infrared and submillimetre line ratios

Redshift-dependent galaxy formation efficiency at z = 5 − 13 in the FirstLight Simulations

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