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arxiv: 2604.20060 · v1 · submitted 2026-04-21 · 🌌 astro-ph.GA · astro-ph.CO· astro-ph.SR· hep-ph

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Unraveling Chemical Enrichment in Extreme Emission-Line Galaxies: A Multi-Element Bayesian View of Bursty Star Formation and Galaxy Evolution in DESI

Razieh Emami , James A. A. Trussler , Tiger Yu-Yang Hsiao , Kaley Brauer , Lars Hernquist , Randall Smith , Douglas Finkbeiner , Fengwu Sun
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Rebecca Davies James F. Steiner Mark Vogelsberger Tobias Looser Grant Tremblay Letizia Bugiani
Authors on Pith no claims yet

Pith reviewed 2026-05-10 01:13 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.COastro-ph.SRhep-ph
keywords extreme emission-line galaxieschemical enrichmentstar formation historiesoutflowsabundance ratiosbayesian modelinggalaxy evolutionbaryon cycle
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The pith

Multi-element abundances in extreme emission-line galaxies serve as a direct probe of rapid baryon cycling in low-mass bursty systems.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper examines 23 nearby extreme emission-line galaxies with strong detections of 19 ionic species, including oxygen, nitrogen, neon, sulfur, and argon. It applies a Bayesian single-zone chemical-evolution model that allows star-formation efficiency, outflow loading, and inflow metallicity to change with time. The fits show short gas depletion timescales and large mass-loading factors, placing these systems in a non-equilibrium regime driven by bursts rather than steady accretion. Abundance ratios separate the effects: star-formation efficiency shapes the overall tracks, outflows control metal retention and normalizations, and inflows set the starting enrichment level. This framework indicates that multi-element data can track how feedback and gas flows operate in small galaxies.

Core claim

We select 23 nearby EELGs with extreme H-alpha and [O III] equivalent widths and detections of 19 ionic species. We infer non-parametric star-formation histories and fit a Bayesian single-zone chemical-evolution model to O, N, Ne, S, and Ar abundances, allowing time-dependent star-formation efficiency, outflow mass loading, and evolving inflow metallicity. The model yields short depletion timescales and large mass-loading factors, indicating rapid gas cycling in a burst-driven non-equilibrium regime below Kennicutt-Schmidt expectations. Abundance ratios isolate drivers, with N/O constraining burst timing and gas flows, Ne/O nearly invariant, and S/O and Ar/O showing intermediate sensitivity.

What carries the argument

A Bayesian single-zone chemical-evolution model fitted simultaneously to O, N, Ne, S, and Ar abundances while allowing time-dependent star-formation efficiency, outflow mass loading, and evolving inflow metallicity.

If this is right

  • Star-formation efficiency sets the evolutionary tracks followed by these galaxies.
  • Outflows regulate metal retention and set the normalization of element-to-oxygen ratios.
  • Inflow metallicity establishes the baseline enrichment level.
  • Nitrogen-to-oxygen ratios provide the strongest constraints on burst timing and gas-flow dynamics.
  • Multi-element abundances can serve as a direct diagnostic of baryon-cycle processes in extreme low-mass starbursts.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The same modeling approach could be applied to larger samples at higher redshift to test whether bursty regimes dominate early chemical enrichment in low-mass systems.
  • If the invariant Ne/O ratio holds across environments, it could act as a stable reference for comparing enrichment histories in different galaxy types.
  • Spatial mapping of multiple elements in these galaxies would test whether the single-zone assumption requires refinement for complex inflow or outflow geometries.

Load-bearing premise

The single-zone chemical-evolution model with time-dependent star-formation efficiency, outflow loading, and inflow metallicity is sufficient to capture the dominant physics without major biases from spatial inhomogeneities or unmodeled processes.

What would settle it

Spatially resolved spectroscopy revealing abundance-ratio variations across a single galaxy that exceed what the single-zone model can produce, or independent gas-mass and star-formation-rate measurements yielding depletion times consistent with equilibrium Kennicutt-Schmidt relations rather than the short values inferred here.

Figures

Figures reproduced from arXiv: 2604.20060 by Douglas Finkbeiner, Fengwu Sun, Grant Tremblay, James A. A. Trussler, James F. Steiner, Kaley Brauer, Lars Hernquist, Letizia Bugiani, Mark Vogelsberger, Randall Smith, Razieh Emami, Rebecca Davies, Tiger Yu-Yang Hsiao, Tobias Looser.

Figure 1
Figure 1. Figure 1: Gallery of our EELG spectra in our DESI sample with stellar masses satisfying 𝑀∗ ≥ 107𝑀⊙. continuity prior (Carnall et al. 2019) to capture rapid, bursty variability without overfitting at early times. We fit DESI Legacy Imaging 𝑔/𝑟/𝑧 photometry, WISE W1/W2, and ten spectrophotometric pseudo-bands constructed from the DESI spectra (following the DR1 VAC approach; DESI Collabora￾tion et al. 2024a; Boquien e… view at source ↗
Figure 2
Figure 2. Figure 2: Inferred star formation histories (SFHs) for the DESI EELG sample derived from our BAGPIPES SED fitting. In each panel, the solid curve shows the median (50th percentile) SFH, while the shaded region denotes the 16th–84th percentile credible interval from the non-parametric posterior distribution. All galaxies display relatively modest star formation at early times followed by a pronounced recent burst tow… view at source ↗
Figure 3
Figure 3. Figure 3: Abundance ratios for the Extremely emission dominated galaxies with 𝑀∗ ≥ 107𝑀⊙ satisfying the criteria in [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: The rest frame EWs for EW(H𝛼) vs EW([O III] 5007). Color-coded we also present 12 + log10 (O/H) for all of galaxies in our sample. 7.7 7.8 7.9 8.0 8.1 8.2 8.3 8.4 12 + log10 (O/H) 10 6.5 10 7.5 10 8.5 10 9.5 M *(M ) 0.5 1.0 1.5 2.0 2.5 S F R(M / y r) [PITH_FULL_IMAGE:figures/full_fig_p010_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Stellar mass (𝑀★) as a function of gas-phase metallicity (12 + log10 (O/H)) for the DESI EELG sample. Points are color￾coded by star formation rate (SFR). The galaxies preferentially lie in the low-metallicity, high-SFR region of parameter space, in agree￾ment with the expected properties of extreme emission-line galaxies. Furthermore, w is defined as the time-scale for a switch from 20% to 80% of stars an… view at source ↗
Figure 6
Figure 6. Figure 6: Representative posterior constraints and best-fit enrichment trajectories for galaxy 𝑁 = 12. The top panel shows the posterior distribution of the five model parameters. The middle and bottom panels show the corresponding best-fit abundance-ratio tracks for the two yield-metallicity assumptions adopted in this work, [M/H] = −1 and 0, respectively. recycled gas to reproduce the observed abundances, whereas … view at source ↗
Figure 7
Figure 7. Figure 7: Constraints on the outflow scaling parameters 𝑛𝜂 and log10 (𝐴𝜂) for the full sample of EELGs. Each panel corresponds to an individual galaxy, showing the median and 16/84 percentiles inferred from the MCMC analysis. Different markers denote results obtained using three SFH realizations from BAGPIPES (16%, 50%, 84% percentiles), while colors distinguish between metallicity assumptions, [M/H] = −1 and 0. The… view at source ↗
Figure 8
Figure 8. Figure 8: Same as [PITH_FULL_IMAGE:figures/full_fig_p014_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Present-day (𝑡𝑜) values of the star formation efficiency timescale 𝜏★, mass-loading factor 𝜂, and inflow metallicity 𝑍in for all galaxies in the EELG sample, derived from the pooled posterior distributions. Each panel shows the median and 16%–84% credible intervals obtained by combining the posterior samples from the three BAGPIPES SFH realizations (16%, 50%, 84% percentiles). Results are shown for two met… view at source ↗
Figure 10
Figure 10. Figure 10 [PITH_FULL_IMAGE:figures/full_fig_p019_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Schematic summary of the parameter dependencies shown in Figure X. Arrows indicate the direction of change in log10 (X/O) versus 12 + log10 (O/H) as each parameter increases. Variations in 𝑛𝜏 and log10 (𝐴𝜏 ) produce diagonal shifts linked to enrichment timescales, while log10 (𝐴𝜂) and 𝑛𝜂 introduce vertical and diagonal displacements associated with outflows. The parameter log10 (𝑍rec) produces an approxim… view at source ↗
Figure 12
Figure 12. Figure 12: Gallery of optical images for the DESI EELG sample with stellar masses satisfying 𝑀∗ ≥ 107𝑀⊙. REFERENCES Amayo, A., Delgado-Inglada, G., & Stasińska, G. 2021, MNRAS, 505, 2361, doi: 10.1093/mnras/stab1467 Andrews, B. H., & Martini, P. 2013, ApJ, 765, 140, doi: 10.1088/0004-637X/765/2/140 Arellano-Córdova, K. Z., Berg, D. A., Chisholm, J., et al. 2022, ApJL, 940, L23, doi: 10.3847/2041-8213/ac9ab2 Arellano… view at source ↗
read the original abstract

Extreme emission-line galaxies (EELGs) probe chemical enrichment in low-mass, bursty systems where star formation, feedback, and gas accretion are poorly constrained. Using DESI DR1, we select 23 nearby EELGs with detections of 19 ionic species (S/N $\geq$ 4), stellar masses $ M_* \geq 10^7 M_{\odot}$, and extreme H$\alpha$ and [O III] 5007 equivalent widths (EW $\geq$ 500 Angstrom). We infer non-parametric star-formation histories and fit a Bayesian single-zone chemical-evolution model to O, N, Ne, S, and Ar, allowing time-dependent star-formation efficiency, outflow mass loading, and evolving inflow metallicity. We find short depletion timescales and large mass-loading factors, indicating rapid gas cycling in a burst-driven, non-equilibrium regime, with depletion times below Kennicutt-Schmidt expectations. Star-formation efficiency and outflows are well constrained, while inflow metallicity is weaker due to degeneracies with metal production. Abundance ratios isolate physical drivers: star-formation efficiency sets evolutionary tracks, outflows regulate metal retention and X/O normalization, and inflow metallicity sets baseline enrichment. N/O strongly constrains burst timing and gas flows, Ne/O remains nearly invariant, and S/O and Ar/O show intermediate sensitivity. These results demonstrate that multi-element abundances provide a direct probe of baryon-cycle processes in extreme low-mass starbursts.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The paper selects 23 nearby EELGs from DESI DR1 with extreme Hα and [O III] equivalent widths (≥500 Å), M* ≥ 10^7 M⊙, and detections of 19 ionic species. It derives non-parametric star-formation histories and fits a Bayesian single-zone chemical-evolution model to O, N, Ne, S, and Ar abundances, allowing time-dependent star-formation efficiency, outflow mass-loading factor, and evolving inflow metallicity. The central results are short depletion timescales and large mass-loading factors indicating rapid, non-equilibrium gas cycling, with abundance ratios (especially N/O) used to isolate drivers of burst timing and baryon flows.

Significance. If the single-zone model recovers unbiased parameters, the work would offer useful constraints on baryon-cycle processes in low-mass bursty systems and demonstrate the diagnostic power of multi-element abundances. The Bayesian treatment of time-dependent parameters and the use of 19 species to break degeneracies are methodological strengths that could be extended to larger samples.

major comments (2)
  1. [model description and results sections] The claim that multi-element abundances provide a 'direct probe' of baryon-cycle processes (abstract) rests on the single-zone model with time-dependent SFE, outflow loading, and inflow metallicity being sufficient. EELGs are selected precisely for extreme burstiness (EW(Hα), [O III] ≥500 Å), where spatial inhomogeneities, patchy enrichment, and non-uniform flows are expected; no explicit test against multi-zone models or hydrodynamical simulations is described to show that inferred depletion times and mass-loading factors remain unbiased under these conditions.
  2. [Bayesian fitting and interpretation paragraphs] The quantitative results (short depletion times below Kennicutt-Schmidt expectations, large mass-loading factors) are outputs of the Bayesian fit to the same abundance data used to constrain the time-dependent parameters. The interpretation that specific ratios (N/O for burst timing, outflows for X/O normalization) isolate physical drivers therefore inherits the fitted values; the manuscript should demonstrate that these conclusions are robust to prior choices and not circular with the model assumptions.
minor comments (2)
  1. The abstract states that inflow metallicity is 'weaker due to degeneracies with metal production' but does not quantify the degeneracy strength or show the posterior correlations; adding a corner plot or degeneracy metric would improve clarity.
  2. The selection criteria (S/N ≥4 for 19 species, EW ≥500 Å) are given but the impact of these cuts on the final sample of 23 galaxies and any post-selection biases are not discussed.

Simulated Author's Rebuttal

2 responses · 1 unresolved

We thank the referee for their insightful comments, which have helped us improve the clarity and robustness of our analysis. We address each major comment below.

read point-by-point responses

  1. Referee: [model description and results sections] The claim that multi-element abundances provide a 'direct probe' of baryon-cycle processes (abstract) rests on the single-zone model with time-dependent SFE, outflow loading, and inflow metallicity being sufficient. EELGs are selected precisely for extreme burstiness (EW(Hα), [O III] ≥500 Å), where spatial inhomogeneities, patchy enrichment, and non-uniform flows are expected; no explicit test against multi-zone models or hydrodynamical simulations is described to show that inferred depletion times and mass-loading factors remain unbiased under these conditions.

    Authors: We recognize that the single-zone model is an approximation, and that EELGs selected for extreme burstiness are expected to exhibit spatial inhomogeneities and non-uniform flows. The integrated nature of the DESI spectra supports the use of a single-zone description as a luminosity-weighted average. Our multi-element approach with 19 species helps constrain the parameters. We have not performed explicit tests against multi-zone models or hydrodynamical simulations, but the results are consistent with other studies of low-mass galaxies. In revision, we will add a dedicated discussion of the model's limitations and potential biases. revision: partial

  2. Referee: [Bayesian fitting and interpretation paragraphs] The quantitative results (short depletion times below Kennicutt-Schmidt expectations, large mass-loading factors) are outputs of the Bayesian fit to the same abundance data used to constrain the time-dependent parameters. The interpretation that specific ratios (N/O for burst timing, outflows for X/O normalization) isolate physical drivers therefore inherits the fitted values; the manuscript should demonstrate that these conclusions are robust to prior choices and not circular with the model assumptions.

    Authors: The model forward predicts abundances from the SFH using the time-dependent parameters, and the data constrain them via the likelihood. Ratios such as N/O are particularly useful because nitrogen enrichment is delayed relative to oxygen, providing a timing constraint somewhat independent of the overall normalization set by outflows. We will revise the manuscript to include explicit demonstrations of robustness to prior choices, such as varying the priors on mass-loading factor and inflow metallicity and showing the impact on the inferred depletion timescales and interpretations. revision: yes

standing simulated objections not resolved
  • Explicit tests of the single-zone model against multi-zone chemical evolution models or hydrodynamical simulations to verify that the inferred depletion times and mass-loading factors are unbiased in the presence of spatial inhomogeneities and patchy enrichment.

Circularity Check

0 steps flagged

No circularity: Bayesian fitting yields independent parameter constraints from abundance data

full rationale

The paper fits a single-zone chemical-evolution model with time-dependent parameters directly to the observed multi-element abundances in the 23 EELGs, then reports the resulting posterior values for depletion time and mass-loading factor as findings. This is standard inference rather than a prediction that reduces to the input data by construction. No self-definitional loops, fitted quantities renamed as predictions, or load-bearing self-citations appear in the provided abstract or derivation outline. The central claim that abundances probe baryon-cycle processes follows from the model interpretation of the fit results, not from any algebraic identity or prior self-citation that forces the outcome. The single-zone assumption is an explicit modeling choice whose adequacy can be tested externally, keeping the derivation self-contained.

Axiom & Free-Parameter Ledger

3 free parameters · 2 axioms · 0 invented entities

The central claim rests on the single-zone assumption, the ability of the Bayesian model to separate star-formation efficiency, outflows, and inflows from abundance ratios, and the representativeness of the 23-galaxy sample for the broader EELG population.

free parameters (3)
  • time-dependent star-formation efficiency
    Allowed to vary freely in the model to match observed abundances and SFHs
  • outflow mass-loading factor
    Time-dependent parameter fitted to regulate metal retention
  • evolving inflow metallicity
    Fitted parameter that sets the baseline enrichment level
axioms (2)
  • domain assumption Single-zone chemical evolution is an adequate description
    Invoked to fit O, N, Ne, S, Ar abundances simultaneously
  • domain assumption Non-parametric star-formation histories can be reliably inferred from the spectra
    Used as input to the chemical-evolution model

pith-pipeline@v0.9.0 · 5642 in / 1549 out tokens · 34540 ms · 2026-05-10T01:13:17.906218+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

94 extracted references · 89 canonical work pages · 3 internal anchors

  1. [1]

    2021, MNRAS, 505, 2361, doi: 10.1093/mnras/stab1467

    Amayo, A., Delgado-Inglada, G., & Stasińska, G. 2021, MNRAS, 505, 2361, doi: 10.1093/mnras/stab1467

    work page doi:10.1093/mnras/stab1467 2021

  2. [2]

    H., & Martini, P

    Andrews, B. H., & Martini, P. 2013, ApJ, 765, 140, doi: 10.1088/0004-637X/765/2/140 Arellano-Córdova, K. Z., Berg, D. A., Chisholm, J., et al. 2022, ApJL, 940, L23, doi: 10.3847/2041-8213/ac9ab2 Arellano-Córdova, K. Z., Berg, D. A., Mingozzi, M., et al. 2024, ApJ, 968, 98, doi: 10.3847/1538-4357/ad34cf

    work page doi:10.1088/0004-637x/765/2/140 2013

  3. [3]

    2022, A&A, 666, A109, doi: 10.1051/0004-6361/202244258

    Arnaboldi, M., Bhattacharya, S., Gerhard, O., et al. 2022, A&A, 666, A109, doi: 10.1051/0004-6361/202244258

    work page doi:10.1051/0004-6361/202244258 2022

  4. [4]

    2011, ApJ, 743, 121, doi: 10.1088/0004-637X/743/2/121 Multi-Element Enrichment in EELGs23

    Atek, H., Siana, B., Scarlata, C., et al. 2011, ApJ, 743, 121, doi: 10.1088/0004-637X/743/2/121 Multi-Element Enrichment in EELGs23

    work page doi:10.1088/0004-637x/743/2/121 2011

  5. [5]

    doi:10.1088/0004-637X/814/1/69 , journal =

    Atek, H., Richard, J., Jauzac, M., et al. 2015, ApJ, 814, 69, doi: 10.1088/0004-637X/814/1/69

    work page doi:10.1088/0004-637x/814/1/69 2015

  6. [6]

    2017, A&A, 608, A1, doi: 10.1051/0004-6361/201730833

    Bacon, R., Conseil, S., Mary, D., et al. 2017, A&A, 608, A1, doi: 10.1051/0004-6361/201730833

    work page doi:10.1051/0004-6361/201730833 2017

  7. [7]

    McQuinn, K. B. W. 2019, ApJ, 874, 93, doi: 10.3847/1538-4357/ab020a

    work page doi:10.3847/1538-4357/ab020a 2019

  8. [8]

    R., Bershady, M

    Blanton, M. R., Bershady, M. A., Abolfathi, B., et al. 2017, AJ, 154, 28, doi: 10.3847/1538-3881/aa7567

    work page doi:10.3847/1538-3881/aa7567 2017

  9. [9]

    M., Barbosa , D., & Liddle , A

    Boissier, S., & Prantzos, N. 1999, MNRAS, 307, 857, doi: 10.1046/j.1365-8711.1999.02699.x

    work page doi:10.1046/j.1365-8711.1999.02699.x 1999

  10. [10]

    2019, A&A, 622, A103, doi: 10.1051/0004-6361/201834156

    Boquien, M., Burgarella, D., Roehlly, Y., et al. 2019, Astronomy and Astrophysics, 622, A103, doi: 10.1051/0004-6361/201834156

    work page internal anchor Pith review doi:10.1051/0004-6361/201834156 2019

  11. [11]

    J., Illingworth, G

    Bouwens, R. J., Illingworth, G. D., Oesch, P. A., et al. 2015, ApJ, 811, 140, doi: 10.1088/0004-637X/811/2/140

    work page doi:10.1088/0004-637x/811/2/140 2015

  12. [12]

    B., et al., 2012, @doi [The Astrophysical Journal Supplement Series] 10.1088/0067-0049/200/2/13 , https://ui.adsabs.harvard.edu/\#abs/2012ApJS..200...13B 200, 13

    Brammer, G. B., van Dokkum, P. G., Franx, M., et al. 2012, ApJS, 200, 13, doi: 10.1088/0067-0049/200/2/13

    work page doi:10.1088/0067-0049/200/2/13 2012

  13. [13]

    C., Leja, J., McLure, R

    Carnall, A. C., Leja, J., McLure, R. J., et al. 2019, Monthly Notices of the Royal Astronomical Society, 490, 417, doi: 10.1093/mnras/stz2339

    work page doi:10.1093/mnras/stz2339 2019

  14. [14]

    C., McLure, R

    Carnall, A. C., McLure, R. J., Dunlop, J. S., & Dave, R. 2018, Monthly Notices of the Royal Astronomical Society, 480, 4379, doi: 10.1093/mnras/sty2169

    work page internal anchor Pith review doi:10.1093/mnras/sty2169 2018

  15. [15]

    , keywords =

    Carniani, S., Hainline, K., D’Eugenio, F., et al. 2024, Nature, 633, 318, doi: 10.1038/s41586-024-07860-9

    work page doi:10.1038/s41586-024-07860-9 2024

  16. [16]

    2025, A&A, 696, A87, doi: 10.1051/0004-6361/202452451

    Carniani, S., D’Eugenio, F., Ji, X., et al. 2025, A&A, 696, A87, doi: 10.1051/0004-6361/202452451

    work page doi:10.1051/0004-6361/202452451 2025

  17. [17]

    Charlot, S., & Fall, S. M. 2000, The Astrophysical Journal, 539, 718, doi: 10.1086/309250

    work page Pith review doi:10.1086/309250 2000

  18. [18]

    , keywords =

    Chiappini, C., Matteucci, F., & Gratton, R. 1997, ApJ, 477, 765, doi: 10.1086/303726

    work page doi:10.1086/303726 1997

  19. [19]

    G., Cardone, V

    Choudhury, T. R., Ferrara, A., & Gallerani, S. 2008, MNRAS, 385, L58, doi: 10.1111/j.1745-3933.2008.00433.x

    work page doi:10.1111/j.1745-3933.2008.00433.x 2008

  20. [20]

    L., Blanton, M

    Coil, A. L., Blanton, M. R., Burles, S. M., et al. 2011, ApJ, 741, 8, doi: 10.1088/0004-637X/741/1/8

    work page doi:10.1088/0004-637x/741/1/8 2011

  21. [21]

    S., White, S

    Colless, M., Dalton, G., Maddox, S., et al. 2001, MNRAS, 328, 1039, doi: 10.1046/j.1365-8711.2001.04902.x Côté, B., O’Shea, B. W., Ritter, C., Herwig, F., & Venn, K. A. 2017, ApJ, 835, 128, doi: 10.3847/1538-4357/835/2/128

    work page doi:10.1046/j.1365-8711.2001.04902.x 2001

  22. [22]

    2011, ApJS, 197, 17, doi: 10.1088/0067-0049/197/2/17

    Cristallo, S., Piersanti, L., Straniero, O., et al. 2011, ApJS, 197, 17, doi: 10.1088/0067-0049/197/2/17

    work page doi:10.1088/0067-0049/197/2/17 2011

  23. [23]

    2025, A&A, 697, A89, doi: 10.1051/0004-6361/202451410

    Curti, M., Witstok, J., Jakobsen, P., et al. 2025, A&A, 697, A89, doi: 10.1051/0004-6361/202451410

    work page doi:10.1051/0004-6361/202451410 2025

  24. [24]

    2023, Nature Astronomy, 7, 622, doi: 10.1038/s41550-023-01918-w

    Curtis-Lake, E., Carniani, S., Cameron, A., et al. 2023, Nature Astronomy, 7, 622, doi: 10.1038/s41550-023-01918-w

    work page doi:10.1038/s41550-023-01918-w 2023

  25. [25]

    S., Schlegel, D

    Dawson, K. S., Schlegel, D. J., Ahn, C. P., et al. 2013, AJ, 145, 10, doi: 10.1088/0004-6256/145/1/10

    work page doi:10.1088/0004-6256/145/1/10 2013

  26. [26]

    , keywords =

    Dawson, K. S., Kneib, J.-P., Percival, W. J., et al. 2016, AJ, 151, 44, doi: 10.3847/0004-6256/151/2/44 DESI Collaboration, Abbas, U., Abdurro’uf, Acosta, A., et al. 2024a, The Astronomical Journal, 168, 58, doi: 10.3847/1538-3881/ad4f1b DESI Collaboration, Abareshi, B., Aguilar, J., et al. 2022, AJ, 164, 207, doi: 10.3847/1538-3881/ac882b DESI Collaborat...

    work page doi:10.3847/0004-6256/151/2/44 2016

  27. [27]

    L., Hägele, G

    Dors, O. L., Hägele, G. F., Cardaci, M. V., et al. 2013, MNRAS, 432, 2512, doi: 10.1093/mnras/stt610

    work page doi:10.1093/mnras/stt610 2013

  28. [28]

    T., & Li, A

    Draine, B. T., & Li, A. 2007, The Astrophysical Journal, 657, 810, doi: 10.1086/511055

    work page doi:10.1086/511055 2007

  29. [29]

    H., Read , M

    Drinkwater, M. J., Jurek, R. J., Blake, C., et al. 2010, MNRAS, 401, 1429, doi: 10.1111/j.1365-2966.2009.15754.x

    work page doi:10.1111/j.1365-2966.2009.15754.x 2010

  30. [30]

    2010, , 405, 1025, 10.1111/j.1365-2966.2010.16486.x

    Driver, S. P., Hill, D. T., Kelvin, L. S., et al. 2011, MNRAS, 413, 971, doi: 10.1111/j.1365-2966.2010.18188.x

    work page doi:10.1111/j.1365-2966.2010.18188.x 2011

  31. [31]

    J., Weinberg, D

    Eisenstein, D. J., Weinberg, D. H., Agol, E., et al. 2011, AJ, 142, 72, doi: 10.1088/0004-6256/142/3/72

    work page doi:10.1088/0004-6256/142/3/72 2011

  32. [32]

    J., Johnson , B

    Eisenstein, D. J., Johnson, B. D., Robertson, B., et al. 2023, arXiv e-prints, arXiv:2310.12340, doi: 10.48550/arXiv.2310.12340

    work page doi:10.48550/arxiv.2310.12340 2023

  33. [33]

    E., García-Rojas, J., et al

    Esteban, C., Méndez-Delgado, J. E., García-Rojas, J., et al. 2025, A&A, 697, A61, doi: 10.1051/0004-6361/202453379

    work page doi:10.1051/0004-6361/202453379 2025

  34. [34]

    L., Bagley, M

    Finkelstein, S. L., Bagley, M. B., Ferguson, H. C., et al. 2023, ApJL, 946, L13, doi: 10.3847/2041-8213/acade4

    work page doi:10.3847/2041-8213/acade4 2023

  35. [35]

    , keywords =

    Gardner, J. P., Mather, J. C., Clampin, M., et al. 2006, SSRv, 123, 485, doi: 10.1007/s11214-006-8315-7

    work page doi:10.1007/s11214-006-8315-7 2006

  36. [36]

    and others , year=

    Gardner, J. P., Mather, J. C., Abbott, R., et al. 2023, PASP, 135, 068001, doi: 10.1088/1538-3873/acd1b5

    work page doi:10.1088/1538-3873/acd1b5 2023

  37. [37]

    Grebel, E. K. 1997, Reviews in Modern Astronomy, 10, 29

    1997

  38. [38]

    2014, A&A, 566, A108, doi: 10.1051/0004-6361/201321489

    Guzzo, L., Scodeggio, M., Garilli, B., et al. 2014, A&A, 566, A108, doi: 10.1051/0004-6361/201321489

    work page doi:10.1051/0004-6361/201321489 2014

  39. [39]

    2023, ApJS, 265, 5, doi: 10.3847/1538-4365/acaaa9 HERA Collaboration, Abdurashidova, Z., Adams, T., et al

    Harikane, Y., Ouchi, M., Oguri, M., et al. 2023, ApJS, 265, 5, doi: 10.3847/1538-4365/acaaa9

    work page doi:10.3847/1538-4365/acaaa9 2023

  40. [40]

    Hodge, P. W. 1971, ARA&A, 9, 35, doi: 10.1146/annurev.aa.09.090171.000343

    work page doi:10.1146/annurev.aa.09.090171.000343 1971

  41. [41]

    Astrophys

    Isobe, Y., Ouchi, M., Tominaga, N., et al. 2023, ApJ, 959, 100, doi: 10.3847/1538-4357/ad09be

    work page doi:10.3847/1538-4357/ad09be 2023

  42. [42]

    2025, MNRAS, 541, L71, doi: 10.1093/mnrasl/slaf056

    Isobe, Y., Maiolino, R., D’Eugenio, F., et al. 2025, MNRAS, 541, L71, doi: 10.1093/mnrasl/slaf056

    work page doi:10.1093/mnrasl/slaf056 2025

  43. [43]

    doi:10.1086/313278

    Iwamoto, K., Brachwitz, F., Nomoto, K., et al. 1999, ApJS, 125, 439, doi: 10.1086/313278

    work page doi:10.1086/313278 1999

  44. [44]

    , keywords =

    Izotov, Y. I., Stasińska, G., Meynet, G., Guseva, N. G., & Thuan, T. X. 2006, A&A, 448, 955, doi: 10.1051/0004-6361:20053763

    work page doi:10.1051/0004-6361:20053763 2006

  45. [45]

    W., & Weinberg, D

    Johnson, J. W., & Weinberg, D. H. 2020, MNRAS, 498, 1364, doi: 10.1093/mnras/staa2431

    work page doi:10.1093/mnras/staa2431 2020

  46. [46]

    W., Weinberg, D

    Johnson, J. W., Weinberg, D. H., Vincenzo, F., et al. 2021, MNRAS, 508, 4484, doi: 10.1093/mnras/stab2718 24Razieh Emami et. al. Jones,D.H., Read,M.A.,Saunders,W., etal.2009,MNRAS, 399, 683, doi: 10.1111/j.1365-2966.2009.15338.x

    work page doi:10.1093/mnras/stab2718 2021

  47. [47]

    2023, ApJL, 951, L17, doi: 10.3847/2041-8213/acd938

    Jones, T., Sanders, R., Chen, Y., et al. 2023, ApJL, 951, L17, doi: 10.3847/2041-8213/acd938

    work page doi:10.3847/2041-8213/acd938 2023

  48. [48]

    S., Hansen, B

    Kalirai, J. S., Hansen, B. M. S., Kelson, D. D., et al. 2008, ApJ, 676, 594, doi: 10.1086/527028

    work page doi:10.1086/527028 2008

  49. [49]

    Makarov, D. I. 2004, AJ, 127, 2031, doi: 10.1086/382905

    work page doi:10.1086/382905 2004

  50. [50]

    Karakas, A. I. 2010, Monthly Notices of the Royal Astronomical Society, 403, 1413, doi: 10.1111/j.1365-2966.2009.16198.x

    work page doi:10.1111/j.1365-2966.2009.16198.x 2010

  51. [51]

    Kennicutt, Jr., R. C. 1998, ApJ, 498, 541, doi: 10.1086/305588

    work page doi:10.1086/305588 1998

  52. [52]

    I., & Lugaro, M

    Kobayashi, C., Karakas, A. I., & Lugaro, M. 2020, ApJ, 900, 179, doi: 10.3847/1538-4357/abae65

    work page doi:10.3847/1538-4357/abae65 2020

  53. [53]

    C., & Kron, R

    Koo, D. C., & Kron, R. G. 1992, ARA&A, 30, 613, doi: 10.1146/annurev.aa.30.090192.003145 Kriek,M., Shapley,A. E.,Reddy, N.A.,et al.2015, ApJS,218, 15, doi: 10.1088/0067-0049/218/2/15 Le Fèvre, O., Vettolani, G., Garilli, B., et al. 2005, A&A, 439, 845, doi: 10.1051/0004-6361:20041960 Le Fèvre, O., Tasca, L. A. M., Cassata, P., et al. 2015, A&A, 576, A79, ...

    work page doi:10.1146/annurev.aa.30.090192.003145 1992

  54. [54]

    J., Carollo, C

    Lilly, S. J., Carollo, C. M., Pipino, A., Renzini, A., & Peng, Y. 2013, ApJ, 772, 119

    2013

  55. [55]

    J., Le Fèvre, O., Renzini, A., et al

    Lilly, S. J., Le Fèvre, O., Renzini, A., et al. 2007, ApJS, 172, 70, doi: 10.1086/516589

    work page doi:10.1086/516589 2007

  56. [56]

    2018, ApJS, 237, 13, doi: 10.3847/1538-4365/aacb24

    Limongi, M., & Chieffi, A. 2018, ApJS, 237, 13, doi: 10.3847/1538-4365/aacb24

    work page doi:10.3847/1538-4365/aacb24 2018

  57. [57]

    , keywords =

    Marques-Chaves, R., Schaerer, D., Kuruvanthodi, A., et al. 2024, A&A, 681, A30, doi: 10.1051/0004-6361/202347411

    work page doi:10.1051/0004-6361/202347411 2024

  58. [58]

    V., van der Wel, A., da Cunha, E., et al

    Maseda, M. V., van der Wel, A., da Cunha, E., et al. 2013, ApJL, 778, L22, doi: 10.1088/2041-8205/778/1/L22

    work page doi:10.1088/2041-8205/778/1/l22 2013

  59. [59]

    V., van der Wel, A., Rix, H.-W., et al

    Maseda, M. V., van der Wel, A., Rix, H.-W., et al. 2014, ApJ, 791, 17, doi: 10.1088/0004-637X/791/1/17

    work page doi:10.1088/0004-637x/791/1/17 2014

  60. [60]

    Mateo, M. L. 1998, ARA&A, 36, 435, doi: 10.1146/annurev.astro.36.1.435

    work page doi:10.1146/annurev.astro.36.1.435 1998

  61. [61]

    Mathis, J. S. 1985, ApJ, 291, 247, doi: 10.1086/163063

    work page doi:10.1086/163063 1985

  62. [62]

    & Bekki, K

    Matteucci, F. 2021, A&A Rv, 29, 5, doi: 10.1007/s00159-021-00133-8

    work page doi:10.1007/s00159-021-00133-8 2021

  63. [63]

    1985, MNRAS, 217, 391, doi: 10.1093/mnras/217.2.391 Miranda-Pérez, B

    Matteucci, F., & Tosi, M. 1985, MNRAS, 217, 391, doi: 10.1093/mnras/217.2.391 Miranda-Pérez, B. E., & Hidalgo-Gámez, A. M. 2023, ApJ, 952, 76, doi: 10.3847/1538-4357/acdb4b

    work page doi:10.1093/mnras/217.2.391 1985

  64. [64]

    2024, , 971, 43, 10.3847/1538-4357/ad5290

    Morishita, T., Stiavelli, M., Grillo, C., et al. 2024, ApJ, 971, 43, doi: 10.3847/1538-4357/ad5290

    work page doi:10.3847/1538-4357/ad5290 2024

  65. [65]

    2023, ApJS, 269, 33, doi: 10.3847/1538-4365/acd556

    Nakajima, K., Ouchi, M., Isobe, Y., et al. 2023, ApJS, 269, 33, doi: 10.3847/1538-4365/acd556

    work page doi:10.3847/1538-4365/acd556 2023

  66. [66]

    2025, arXiv e-prints, arXiv:2503.11457, doi: 10.48550/arXiv.2503.11457

    Nakane, M., Ouchi, M., Nakajima, K., et al. 2025, arXiv e-prints, arXiv:2503.11457, doi: 10.48550/arXiv.2503.11457

    work page doi:10.48550/arxiv.2503.11457 2025

  67. [67]

    Pagel, B. E. J. 1997, Nucleosynthesis and Chemical Evolution of Galaxies

    1997

  68. [68]

    1969, Boletin de los Observatorios Tonantzintla y Tacubaya, 5, 3

    Peimbert, M., & Costero, R. 1969, Boletin de los Observatorios Tonantzintla y Tacubaya, 5, 3

    1969

  69. [69]

    1977, MNRAS, 179, 217, doi: 10.1093/mnras/179.2.217

    Peimbert, M., & Torres-Peimbert, S. 1977, MNRAS, 179, 217, doi: 10.1093/mnras/179.2.217

    work page doi:10.1093/mnras/179.2.217 1977

  70. [70]

    I., van der Werf, P

    Pelupessy, F. I., van der Werf, P. P., & Icke, V. 2004, A&A, 422, 55, doi: 10.1051/0004-6361:20047071 Pérez-Montero, E., Hägele, G. F., Contini, T., & Díaz, Á. I. 2007, MNRAS, 381, 125, doi: 10.1111/j.1365-2966.2007.12213.x

    work page doi:10.1051/0004-6361:20047071 2004

  71. [71]

    2019, ApJ, 874, 125, doi: 10.3847/1538-4357/ab08ec

    Pharo, J., Malhotra, S., Rhoads, J., et al. 2019, ApJ, 874, 125, doi: 10.3847/1538-4357/ab08ec

    work page doi:10.3847/1538-4357/ab08ec 2019

  72. [72]

    J., Robertson, B., Tacchella, S., et al

    Rieke, M. J., Robertson, B., Tacchella, S., et al. 2023, ApJS, 269, 16, doi: 10.3847/1538-4365/acf44d

    work page doi:10.3847/1538-4365/acf44d 2023

  73. [73]

    , keywords =

    Robertson, B., Johnson, B. D., Tacchella, S., et al. 2024, ApJ, 970, 31, doi: 10.3847/1538-4357/ad463d

    work page doi:10.3847/1538-4357/ad463d 2024

  74. [74]

    , keywords =

    Robertson, B. E., Ellis, R. S., Furlanetto, S. R., & Dunlop, J. S. 2015, ApJL, 802, L19, doi: 10.1088/2041-8205/802/2/L19

    work page doi:10.1088/2041-8205/802/2/l19 2015

  75. [75]

    Rogers, N. S. J., Strom, A. L., Rudie, G. C., et al. 2024, ApJL, 964, L12, doi: 10.3847/2041-8213/ad2f37

    work page doi:10.3847/2041-8213/ad2f37 2024

  76. [76]

    R., & Kunth, D

    Roy, J. R., & Kunth, D. 1995, A&A, 294, 432, doi: 10.48550/arXiv.astro-ph/9410023

    work page internal anchor Pith review doi:10.48550/arxiv.astro-ph/9410023 1995

  77. [77]

    2014, MNRAS, 437, L26, doi: 10.1093/mnrasl/slt132

    Salvadori, S., Tolstoy, E., Ferrara, A., & Zaroubi, S. 2014, MNRAS, 437, L26, doi: 10.1093/mnrasl/slt132

    work page doi:10.1093/mnrasl/slt132 2014

  78. [78]

    L., Shapley , A

    Sanders, R. L., Shapley, A. E., Reddy, N. A., et al. 2020, MNRAS, 491, 1427, doi: 10.1093/mnras/stz3032

    work page doi:10.1093/mnras/stz3032 2020

  79. [79]

    Sargent, W. L. W. 1970, ApJ, 160, 405, doi: 10.1086/150443

    work page doi:10.1086/150443 1970

  80. [80]

    , year = 1959, month = mar, volume =

    Schmidt, M. 1959, ApJ, 129, 243, doi: 10.1086/146614 —. 1963, ApJ, 137, 758, doi: 10.1086/147553

    work page doi:10.1086/146614 1959

Showing first 80 references.