Spatially resolved gas-phase metallicity in FIRE-2 dwarfs: late-time evolution of metallicity relations in simulations with feedback and mergers

Porter, Lori; Orr, M.; Burkhart, Blakesley; Wetzel, Andrew; Ma, Xiangcheng; Hopkins, Philip F.; Emerick, Andrew

doi:10.1093/mnras/stac1958

Cited by 5 publications

(1 citation statement)

References 115 publications

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“…Many Observations and simulations have shown that most galaxies tend to have negative metallicity gradients (Edmunds & Greenhow 1995;van Zee et al 1998;Mollá et al 1999;Kewley et al 2010;Belfiore et al 2017;Hemler et al 2021;Porter et al 2022), which is consistent with the inside-out galaxy formation (Mo et al 1998;Pilkington et al 2012;Sharda et al 2021). Early star formation rapidly increases the metallicity in the central region of a galaxy, while the outer disk increases in metallicity more slowly.…”

Section: Possible Mechanisms Of the Formation Of Sf-etgsmentioning

confidence: 70%

The Origin of Star Formation in Early-type Galaxies Inferred from Spatially Resolved Spectroscopy

Lee

Hwang

et al. 2023

ApJ

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We investigate the origin of star formation activity in early-type galaxies with current star formation using spatially resolved spectroscopic data from the Mapping Nearby Galaxies at Apache Point Observatory in the Sloan Digital Sky Survey (SDSS). We first identify star-forming early-type galaxies from the SDSS sample, which are morphologically early-type but show current star formation activity in their optical spectra. We then construct comparison samples with different combinations of star formation activity and morphology, which include star-forming late-type galaxies, quiescent early-type galaxies, and quiescent late-type galaxies. Our analysis of the optical spectra reveals that the star-forming early-type galaxies have two distinctive episodes of star formation, which is similar to late-type galaxies but different from quiescent early-type galaxies with a single star formation episode. Star-forming early-type galaxies have properties in common with star-forming late-type galaxies, which include stellar population, gas and dust content, mass, and environment. However, the physical properties of star-forming early-type galaxies derived from spatially resolved spectroscopy differ from those of star-forming late-type galaxies in the sense that the gas in star-forming early-type galaxies is more concentrated than their stars, and is often kinematically misaligned with stars. The age gradient of star-forming early-type galaxies also differs from those of star-forming late-type galaxies. Our findings suggest that the current star formation in star-forming early-type galaxies has an external origin including galaxy mergers or accretion gas from the cosmic web.

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Section: Possible Mechanisms Of the Formation Of Sf-etgsmentioning

confidence: 70%

The Origin of Star Formation in Early-type Galaxies Inferred from Spatially Resolved Spectroscopy

Lee

Hwang

et al. 2023

ApJ

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JADES: Detecting [OIII]λ4363 emitters and testing strong line calibrations in the high-z Universe with ultra-deep JWST/NIRSpec spectroscopy up to z ∼ 9.5

Laseter,

Maseda,

Curti

et al. 2024

A&A

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We present ten novel [OIII]λ4363 auroral line detections up to z ∼ 9.5 measured from ultra-deep JWST/NIRSpec MSA spectroscopy from the JWST Advanced Deep Extragalactic Survey (JADES). We leverage the deepest spectroscopic observations taken thus far with NIRSpec to determine electron temperatures and oxygen abundances using the direct Te method. We directly compare these results against a suite of locally calibrated strong-line diagnostics and recent high-z calibrations. We find the calibrations fail to simultaneously match our JADES sample, thus warranting a self-consistent revision of these calibrations for the high-z Universe. We find a weak dependence between R2 and O3O2 with metallicity, thus suggesting these line ratios are inefficient in the high-z Universe as metallicity diagnostics and degeneracy breakers. We find R3 and R23 are still correlated with metallicity, but we find a tentative flattening of these diagnostics, thus suggesting future difficulties when applying these strong line ratios as metallicity indicators in the high-z Universe. We also propose and test an alternative diagnostic based on a different combination of R3 and R2 with a higher dynamic range. We find a reasonably good agreement (median offset of 0.002 dex, median absolute offset of 0.13 dex) with the JWST sample at low metallicity, but future investigations are required on larger samples to probe past the turnover point. At a given metallicity, our sample demonstrates higher ionization and excitation ratios than local galaxies with rest-frame EWs(Hβ) ≈200 − 300 Å. However, we find the median rest-frame EWs(Hβ) of our sample to be ∼2× less than the galaxies used for the local calibrations. This EW discrepancy combined with the high ionization of our galaxies does not offer a clear description of [OIII]λ4363 production in the high-z Universe, thus warranting a much deeper examination into the factors influencing these processes.

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The internal metallicity distributions of simulated galaxies from EAGLE, Illustris, and IllustrisTNG at z = 1.8–4 as probed by gamma-ray burst hosts

Metha

Trenti

2023

Monthly Notices of the Royal Astronomical Society

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Massive stars are thought to be progenitors of Long Gamma Ray Bursts (GRBs), most likely with a bias favouring low metallicity progenitors. Because galaxies do not have a constant metallicity throughout, the combination of line-of-sight absorption metallicity inferred from GRB afterglow spectroscopy and of host galaxy global metallicity derived from emission lines diagnostics represents a powerful way to probe both the bias function for GRB progenitors, and the chemical inhomogeneities across star forming regions. In this study, we predict the relationship between Zabs and Zemiss using three different hydrodynamical cosmological simulations: Illustris, EAGLE, and IllustrisTNG. We find that while the qualitative shape of the curve relating emission versus absorption metallicity remains the same, the predicted relationship between these two observables is significantly different between the simulations. Using data for the host galaxy of GRB121024A for which both Zabs and Zemiss have been measured, we find marginal support for the Illustris simulation as producing the most-realistic internal metallicity distributions within star-forming galaxies at cosmic noon. Overall, all simulations predict similar properties for the bulk of the GRB host galaxy population, but each has distinct features in the tail of the Zabs-Zemiss distribution that in principle allow to discriminate between models if a sufficiently large sample of observations are available (i.e. N ≳ 11 on average). Substantial progress is expected in the near future, with upcoming JWST/NIRspec observations of 10 GRB host galaxies for which absorption metallicity from the afterglow spectra exists.

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Spatially resolved gas-phase metallicity in FIRE-2 dwarfs: late-time evolution of metallicity relations in simulations with feedback and mergers

Cited by 5 publications

References 115 publications

The Origin of Star Formation in Early-type Galaxies Inferred from Spatially Resolved Spectroscopy

The Origin of Star Formation in Early-type Galaxies Inferred from Spatially Resolved Spectroscopy

JADES: Detecting [OIII]λ4363 emitters and testing strong line calibrations in the high-z Universe with ultra-deep JWST/NIRSpec spectroscopy up to z ∼ 9.5

The internal metallicity distributions of simulated galaxies from EAGLE, Illustris, and IllustrisTNG at z = 1.8–4 as probed by gamma-ray burst hosts

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