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arxiv: 2605.06769 · v1 · submitted 2026-05-07 · 🌌 astro-ph.GA

Recognition: 2 theorem links

· Lean Theorem

Origins of Extreme Emission-Line Ratios in z > 3 Galaxies: Insights from the Lumen Model

Lucie Scharr\'e , Michaela Hirschmann , Ad\`ele Plat , Stephane Charlot , Rachel S. Somerville , Emma Curtis-Lake , Gabriella De Lucia , Miroslava Dessauges-Zavadsky
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Anna Feltre Marion Farcy Natalia Lah\'en Aswin P. Vijayan Stephen M. Wilkins
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Pith reviewed 2026-05-11 00:45 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords high-redshift galaxiesemission-line ratiosHII regionsionization parameternitrogen abundanceBPT diagramstar-forming galaxiesnebular modeling
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The pith

Models with harder ionizing spectra, high ionization from massive star clusters, and enhanced nitrogen reproduce extreme emission-line ratios in z>3 galaxies.

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

The paper introduces Lumen, a framework that places HII regions with realistic properties throughout galaxies in cosmological simulations and computes their combined emission lines. It applies this to IllustrisTNG50 galaxies at redshifts 3 to 8 and tests proposed causes for the strong offsets in ratios such as [OIII]/Hβ and [OIII]/[OII] compared with local galaxies. The authors show that alpha-enhancement by itself is insufficient, but the combination of harder stellar spectra, ionization parameters boosted by clusters of 10^5 to 10^6 solar masses, and higher nitrogen abundances matches the observed positions across the N2-BPT, S2-VO87, and O32-R23 diagrams. A reader would care because these conditions point to distinct star-formation and enrichment processes in the early universe and supply updated tools for classifying distant galaxies observed by JWST.

Core claim

Lumen models spatially distributed HII regions inside IllustrisTNG50 and finds that the most extreme [OIII]/Hβ and [OIII]/[OII] values require high ionization parameters powered by massive star clusters, while the highest [NII]/Hα ratios additionally need enhanced nitrogen abundances; when these are combined with harder ionizing spectra the full high-redshift population is reproduced on three diagnostic diagrams, which in turn motivates new demarcation lines separating star-forming galaxies from AGN.

What carries the argument

The Lumen framework, which generates a population of HII regions with properties drawn from the simulation, computes their individual nebular spectra with photoionization models, and sums them to obtain integrated line ratios.

If this is right

  • Moderate line-ratio offsets arise from alpha-enhancement together with a higher IMF upper-mass cutoff and AGN contributions, without needing extreme densities.
  • Gas densities near 10^4 cm^-3 can increase several ratios but suppress [SII]/Hα, placing them in tension with current data.
  • Massive star clusters of 10^5-10^6 solar masses are required to reach the highest ionization parameters consistent with recent JWST observations.
  • New demarcation lines in the N2-BPT and S2-VO87 diagrams better isolate star-forming galaxies at high redshift.

Where Pith is reading between the lines

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

  • The emphasis on clustered star formation suggests that higher-resolution imaging or simulations should detect more such massive clusters in distant galaxies.
  • The requirement for rapid nitrogen enrichment implies that chemical-evolution models must incorporate efficient nitrogen production channels at early times.
  • Extending the same Lumen-style post-processing to other cosmological simulations would test how sensitive the conclusions are to the underlying galaxy-formation physics.

Load-bearing premise

The spatial distribution and clustering of massive star-forming regions generated by Lumen inside IllustrisTNG50 accurately represent the structure of real high-redshift galaxies.

What would settle it

A sample of z>3 galaxies with the most extreme observed line ratios that lack star clusters above 10^5 solar masses or show normal nitrogen abundances would contradict the explanation.

Figures

Figures reproduced from arXiv: 2605.06769 by Ad\`ele Plat, Anna Feltre, Aswin P. Vijayan, Emma Curtis-Lake, Gabriella De Lucia, Lucie Scharr\'e, Marion Farcy, Michaela Hirschmann, Miroslava Dessauges-Zavadsky, Natalia Lah\'en, Rachel S. Somerville, Stephane Charlot, Stephen M. Wilkins.

Figure 1
Figure 1. Figure 1: Compilation of star-forming galaxy observations between 𝑧 = 1.4 and 𝑧 = 9.4 in the N2-BPT (left), S2-VO87 (middle), and the O32–R23 (right) diagram, as indicated in the legend. For comparison included are local SDSS-observed galaxies (black outline), the theoretical upper limits for star-forming galaxies (Kewley et al. 2001a, dotted lines) and the empirical lower limit for AGN (Kauffmann et al. 2003, dashe… view at source ↗
Figure 2
Figure 2. Figure 2: Lumen method illustrated for one example galaxy at 𝑧 = 0 in the Base model. The initial positions of young star particles formed in IllustrisTNG (blue stars, top left) are resampled into young star clusters (circular data points, bottom left) and reinserted into the dense gas. Based on the metallicity (top middle) and the ionization parameter (bottom middle), photoionization models coupled to each cluster … view at source ↗
Figure 3
Figure 3. Figure 3: Comparison of physical properties of H ii regions from the PHANGS catalogue (orange) and in the Lumen 𝑧 = 0 sample (blue). Shown are the ionization parameter (left), circularised PHANGS radii and Lumen Strömgren radii (middle), and H𝛼 luminosity (right). underrepresented in PHANGS due to sample limitations (168 pre￾dicted by Lumen across all 6627 galaxies), artificially fragmented into multiple subregions,… view at source ↗
Figure 4
Figure 4. Figure 4: Location of Lumen H ii regions in the galaxy from [PITH_FULL_IMAGE:figures/full_fig_p011_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Location of Lumen galaxy populations at 𝑧 = 0 in different line-ratio diagrams, N2-BPT (top left), S2-VO87 (top right), and [O i]𝜆6300/H𝛼-VO87 (bottom left), as well as O32–R23 (bottom right). Shown are simulated galaxies above a mass cut of 108 M⊙ with line luminosities limited to 1039 erg s−1 (dark blue contours), as well as an extended population down to 107 M⊙ with no luminosity limit (light blue conto… view at source ↗
Figure 6
Figure 6. Figure 6: Lumen predictions for galaxies at 𝑧 = 0 for the H𝛼 luminosity function (top left), as well as local scaling relations for SFR (centre and bottom left) and gas-phase metallicity (centre and right columns). Simulated galaxies are shown for mass cuts of 108 M⊙ (solid blue) and 107 M⊙ (dotted blue with 1𝜎 scatter). Observational determinations are shown for the H𝛼 luminosity function (orange lines, Ly et al. 2… view at source ↗
Figure 7
Figure 7. Figure 7: Location of galaxy populations at 𝑧 = 3–8 from Lumen models (light and dark blue scatter, flux-limited to 10−19 erg s−1 cm−2 ) in the classical N2-BPT diagram. Lumen variations shown are: Base model (top left), BPASS (top middle), high IMF upper mass cut (top right), 𝛼-enhancement (middle left), high IMF upper mass cut and 𝛼-enhancement combined (centre), weak and strong AGN (middle right), increased minim… view at source ↗
Figure 8
Figure 8. Figure 8: Location of galaxy populations at 𝑧 = 3–8 from the same Lumen models as in [PITH_FULL_IMAGE:figures/full_fig_p016_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Location of galaxy populations at 𝑧 = 3–8 of Lumen models (blue data points, flux-limited to 10−19 erg s−1 cm−2 ) in the O32–R23 diagram. Shown are the Base model (top left), BPASS (top middle), high IMF upper mass cut (top right), 𝛼-enhancement (middle left), high IMF upper mass cut and 𝛼-enhancement combined (centre), weak and strong AGN (middle right), increased minimum cluster masses to 105 and 106 M⊙ … view at source ↗
Figure 10
Figure 10. Figure 10: Location of galaxy populations at 𝑧 = 3–8 from Lumen Base and “Master” models (grey contours and blue data points, respectively, flux-limited to 10−19 erg s−1 cm−2 ) in the N2-BPT (left), S2-VO87 (middle), and the O32–R23 (right) diagram against observations between 𝑧 = 2.5–9.4 (orange). In addition to the classical classification lines from Kewley et al. (2001b) and Kauffmann et al. (2003), new demarcati… view at source ↗
Figure 11
Figure 11. Figure 11: Luminosity functions from 𝑧 = 3 to 8 for H𝛼 (top row) and [O iii]𝜆5007 (bottom row), as predicted by the Base (dark blue) and “Master” (light blue) Lumen models, compared to dust-corrected observational constraints (orange): H𝛼 from Covelo-Paz et al. (2025, solid); [O iii]𝜆5007 from Khostovan et al. (2015, dashed) and Meyer et al. (2024, 2025, dash-dotted), respectively, with an additional extrapolation f… view at source ↗
Figure 12
Figure 12. Figure 12: R3 (purple) and O32 (orange) value distribution for Lumen models between 𝑧 = 3–8 (boxplots, outlier points in black circles) compared to the highest observed R3 between 𝑧 = 2.7–7.5 and O32 values between 𝑧 = 2.7–9.4 (horizontal lines). Shown are the 90th percentiles (thick solid lines) and values above this threshold (thin dashed lines). The maximum (grey dashed line) and average (grey solid line) log𝑈 of… view at source ↗
Figure 13
Figure 13. Figure 13: Same as [PITH_FULL_IMAGE:figures/full_fig_p022_13.png] view at source ↗
read the original abstract

Optical emission-line ratios in star-forming galaxies at $z \sim 3$-8, such as [OIII]/H$\beta$ and [OIII]/[OII], are strongly offset from those at $z \sim 0$-2, pointing to more extreme ionization and ISM conditions in the early Universe. To constrain the physical origin of these offsets, we developed Lumen, a framework for modelling nebular emission from spatially distributed HII regions in cosmological simulations. We apply Lumen to IllustrisTNG50, validate its predictions at low redshift, and test a suite of proposed mechanisms for producing extreme line ratios at $z = 3$-8. We focus on the [NII]/H$\alpha$ versus [OIII]/H$\beta$ (N2-BPT) diagram, the [SII]/H$\alpha$ versus [OIII]/H$\beta$ (S2-VO87) diagram, and the [OIII]/[OII] versus ([OII]+[OIII])/H$\beta$ (O32-R23) diagram. We find that $\alpha$-enhancement alone cannot explain the bulk of observations. Moderate offsets emerge from the combined effects of $\alpha$-enhancement, a higher IMF upper-mass cutoff, and AGN contributions. The most extreme [OIII]/H$\beta$ and [OIII]/[OII] values require high ionization parameters powered by massive star clusters of $\gtrsim 10^5$-$10^6\,\mathrm{M}_\odot$, consistent with recent JWST observations. Reproducing the highest [NII]/H$\alpha$ ratios additionally requires enhanced nitrogen abundances. Although gas densities of $n \sim 10^4\,\mathrm{cm}^{-3}$ can boost several diagnostic ratios, they suppress [SII]/H$\alpha$ and are therefore in tension with current observations. Overall, models combining harder ionizing spectra, elevated ionization parameters from massive star clusters, and enhanced nitrogen abundances reproduce the observed high-$z$ galaxy population across the N2-BPT, S2-VO87, and O32-R23 diagrams. This successful model also motivates new demarcation lines for star-forming galaxies in the N2-BPT and S2-VO87 diagrams.

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

3 major / 2 minor

Summary. The paper introduces the Lumen framework for modeling nebular emission from spatially distributed HII regions embedded in the IllustrisTNG50 cosmological simulation. After low-redshift validation, the authors systematically test proposed mechanisms (α-enhancement, harder spectra, elevated ionization parameter U from massive clusters, enhanced nitrogen, high gas density, AGN) for the observed offsets in z>3 galaxies on the N2-BPT, S2-VO87, and O32-R23 diagrams. They conclude that only the combination of harder ionizing spectra, high-U powered by ≳10^5–10^6 M⊙ clusters, and enhanced N abundances reproduces the full set of extreme line ratios, while α-enhancement alone is insufficient and high densities are in tension with [SII] data; new demarcation lines are proposed.

Significance. If the modeling chain holds, the work supplies a physically grounded account of why high-z emission-line ratios are extreme, isolates the necessary role of massive star-cluster-driven ionization and N enrichment, and supplies new diagnostic boundaries. It directly connects sub-grid ISM physics in large-volume simulations to JWST observables and offers falsifiable predictions for future cluster-scale observations.

major comments (3)
  1. [Methods (Lumen framework)] Methods (Lumen HII-region placement): The headline result that high ionization parameters from ≳10^5–10^6 M⊙ clusters are required rests on Lumen’s sub-grid mapping of TNG50 star particles. Because TNG50’s baryonic resolution (~8×10^4 M⊙) does not resolve <100 pc clustering, the high-U tail is an output of the chosen cluster-mass and spatial-distribution assumptions rather than an emergent prediction; no sensitivity test varying the volume-filling factor or luminosity-weighted U prescription is shown to demonstrate robustness.
  2. [Results (N2-BPT, O32-R23)] Results (N2-BPT and O32-R23 panels): The necessity of enhanced nitrogen is demonstrated only after the high-U channel is already included; the paper does not quantify the minimum N enhancement required or test whether the same extreme ratios can be recovered with a different combination (e.g., higher U plus modest AGN contribution) without N enhancement.
  3. [Validation] Validation section: Low-redshift validation is reported, but the manuscript does not show whether the same Lumen parameter choices that reproduce z~0 line ratios also produce the high-U tail at z>3, or whether retuning is required; this leaves open the possibility that the high-z success is partly post-hoc.
minor comments (2)
  1. [Figures] Figure captions for the diagnostic diagrams should explicitly state the redshift range and selection cuts applied to both the simulated and observed samples for each panel.
  2. [Results] The abstract states that gas densities n~10^4 cm^{-3} suppress [SII]/Hα; the corresponding quantitative prediction (e.g., the factor by which [SII]/Hα drops) should be shown in a dedicated panel or table.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed comments, which help clarify key aspects of our modeling framework and strengthen the presentation of results. We address each major comment below and indicate the revisions planned for the next version of the manuscript.

read point-by-point responses

  1. Referee: [Methods (Lumen framework)] Methods (Lumen HII-region placement): The headline result that high ionization parameters from ≳10^5–10^6 M⊙ clusters are required rests on Lumen’s sub-grid mapping of TNG50 star particles. Because TNG50’s baryonic resolution (~8×10^4 M⊙) does not resolve <100 pc clustering, the high-U tail is an output of the chosen cluster-mass and spatial-distribution assumptions rather than an emergent prediction; no sensitivity test varying the volume-filling factor or luminosity-weighted U prescription is shown to demonstrate robustness.

    Authors: We agree that the high-U tail depends on our sub-grid assumptions for cluster masses and spatial distributions, given TNG50's resolution limits. In the revised manuscript we will add an appendix with sensitivity tests that vary the cluster mass function slope and the HII-region volume-filling factor. These tests will show that the requirement for ≳10^5–10^6 M⊙ clusters to reach the most extreme observed ratios remains robust across plausible variations, while we will also expand the methods text to explicitly discuss the limitations of the sub-grid approach and the luminosity-weighted U prescription. revision: yes

  2. Referee: [Results (N2-BPT, O32-R23)] Results (N2-BPT and O32-R23 panels): The necessity of enhanced nitrogen is demonstrated only after the high-U channel is already included; the paper does not quantify the minimum N enhancement required or test whether the same extreme ratios can be recovered with a different combination (e.g., higher U plus modest AGN contribution) without N enhancement.

    Authors: We acknowledge that the current presentation does not isolate the minimum N enhancement or fully explore alternative combinations. In the revision we will add new model grids that (i) quantify the lowest N enhancement factor needed to reproduce the highest [NII]/Hα ratios once high-U is fixed, and (ii) test whether elevated U combined with modest AGN contributions (but no N enhancement) can recover the same extreme ratios. These additional runs will be shown in the results section and will demonstrate that N enhancement remains necessary for the upper envelope of the observed [NII]/Hα distribution. revision: yes

  3. Referee: [Validation] Validation section: Low-redshift validation is reported, but the manuscript does not show whether the same Lumen parameter choices that reproduce z~0 line ratios also produce the high-U tail at z>3, or whether retuning is required; this leaves open the possibility that the high-z success is partly post-hoc.

    Authors: We thank the referee for highlighting this point. The Lumen parameters were held fixed after low-z validation and applied directly to the z>3 snapshots. In the revised manuscript we will add a direct comparison (new figure panel in the validation section) of the ionization-parameter distribution at z>3 using exactly the same parameter set as the z~0 models. This will confirm that the high-U tail emerges naturally from the higher star-formation activity and more massive star particles present at high redshift, without any retuning. revision: yes

Circularity Check

0 steps flagged

No significant circularity in Lumen framework or high-z line ratio modeling

full rationale

The paper introduces the Lumen framework for spatially distributed HII region emission and applies it to the external IllustrisTNG50 simulation. It validates low-redshift predictions and tests physical mechanisms (harder spectra, high ionization parameters from massive clusters, enhanced N) against observed high-z diagnostics without any equations or steps that reduce the target line ratios (N2-BPT, S2-VO87, O32-R23) to quantities fitted from the high-z data itself. No self-citations are load-bearing for the central claim, no ansatzes are smuggled, and no uniqueness theorems or renamings create self-referential loops. The derivation chain remains independent and externally benchmarked.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The central claim rests on the accuracy of the IllustrisTNG50 galaxy population, the mapping from stellar populations to ionizing spectra inside Lumen, and the assumption that the chosen ionization-parameter and abundance adjustments are physically plausible rather than purely tuned.

free parameters (2)
  • ionization parameter
    Elevated values powered by massive star clusters are required to reach the highest [OIII]/Hβ and [OIII]/[OII] ratios.
  • nitrogen abundance enhancement
    Additional N enhancement is invoked to reproduce the highest [NII]/Hα ratios.
axioms (1)
  • domain assumption IllustrisTNG50 provides a sufficiently realistic spatial distribution of HII regions at z=3-8
    The entire exercise depends on the simulation's star-formation and feedback prescriptions.

pith-pipeline@v0.9.0 · 5792 in / 1412 out tokens · 37346 ms · 2026-05-11T00:45:16.201362+00:00 · methodology

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Works this paper leans on

295 extracted references · 274 canonical work pages · 4 internal anchors

  1. [1]

    and Chevallard, Jacopo and Choi, Ena and Nelson, Dylan and Morisset, Christophe and Plat, Adele and Vidal-Garcia, Alba , number =

    Hirschmann, Michaela and Charlot, Stephane and Feltre, Anna and Curtis-Lake, Emma and Somerville, Rachel S. and Chevallard, Jacopo and Choi, Ena and Nelson, Dylan and Morisset, Christophe and Plat, Adele and Vidal-Garcia, Alba , number =. 2023 , journal =. doi:10.1093/mnras/stad2955 , issn =

    work page doi:10.1093/mnras/stad2955 2023

  2. [2]

    , number =

    Hirschmann, Michaela and Charlot, Stephane and Somerville, Rachel S. , number =. 2023 , journal =. doi:10.1093/MNRAS/STAD2745 , issn =

    work page doi:10.1093/mnras/stad2745 2023

  3. [3]

    and Coil, Alison L

    Liu, Xin and Shapley, Alice E. and Coil, Alison L. and Brinchmann, Jarle and Ma, Chung‐Pei , number =. 2008 , journal =. doi:10.1086/529030 , issn =

    work page doi:10.1086/529030 2008

  4. [4]

    and Fischera, Jorg and Sutherland, Ralph S

    Dopita, Michael A. and Fischera, Jorg and Sutherland, Ralph S. and Kewley, Lisa J. and Leitherer, Claus and Tuffs, Richard J. and Popescu, Cristina C. and van Breugel, Wil and Groves, Brent A. , number =. 2006 , journal =. doi:10.1086/508261/FULLTEXT/ , issn =

    work page doi:10.1086/508261/fulltext/ 2006

  5. [5]

    and Fischera, Jorg and Sutherland, Ralph S

    Dopita, Michael A. and Fischera, Jorg and Sutherland, Ralph S. and Kewley, Lisa J. and Tuffs, Richard J. and Popescu, Cristina C. and van Breugel, Wil and Groves, Brent A. and Leitherer, Claus , number =. 2006 , journal =. doi:10.1086/505418/FULLTEXT/ , issn =

    work page doi:10.1086/505418/fulltext/ 2006

  6. [6]

    and Lilly, S

    Maier, C. and Lilly, S. J. and Carollo, C. M. and Meisenheimer, K. and Hippelein, H. and Stockton, A. , number =. 2006 , journal =. doi:10.1086/499518/FULLTEXT/ , issn =

    work page doi:10.1086/499518/fulltext/ 2006

  7. [7]

    2013 , journal =

    Cielo, S and Antonuccio-Delogu, V and Macci. 2013 , journal =

    2013

  8. [8]

    and Kodama, Tadayuki and Komiyama, Yutaka and Leauthaud, Alexie and Lin, Yen Ting and Miyazaki, Satoshi and Nagao, Tohru and Nishizawa, Atsushi J

    Hayashi, Masao and Tanaka, Masayuki and Shimakawa, Rhythm and Furusawa, Hisanori and Momose, Rieko and Koyama, Yusei and Silverman, John D. and Kodama, Tadayuki and Komiyama, Yutaka and Leauthaud, Alexie and Lin, Yen Ting and Miyazaki, Satoshi and Nagao, Tohru and Nishizawa, Atsushi J. and Ouchi, Masami and Shibuya, Takatoshi and Tadaki, Ken Ichi and Yabe...

    work page doi:10.1093/pasj/psx088 2018

  9. [9]

    doi:10.1093/mnras/stz2278 , arxivId =

    2019 , author =. doi:10.1093/mnras/stz2278 , arxivId =

    work page doi:10.1093/mnras/stz2278 2019

  10. [10]

    1985 , booktitle =

    POLLACK ANt CHRISTOPHER P McKAY, James B and Christofferson, Bruce M , pages =. 1985 , booktitle =

    1985

  11. [11]

    L., Finkelstein, S

    2023 , author =. doi:10.3847/2041-8213/ace619 , arxivId =

    work page doi:10.3847/2041-8213/ace619 2023

  12. [12]

    doi:10.1093/mnras/stae2723 , arxivId =

    2025 , author =. doi:10.1093/mnras/stae2723 , arxivId =

    work page doi:10.1093/mnras/stae2723 2025

  13. [13]

    R., & Gnedin, N

    Krumholz, Mark R. and Gnedin, Nickolay Y. , number =. 2011 , journal =. doi:10.1088/0004-637X/729/1/36 , issn =

    work page doi:10.1088/0004-637x/729/1/36 2011

  14. [14]

    and Schaye, Joop and Crain, Robert A

    Turner, Monica L. and Schaye, Joop and Crain, Robert A. and Rudie, Gwen and Steidel, Charles C. and Strom, Allison and Theuns, Tom , number =. 2017 , journal =. doi:10.1093/MNRAS/STX1616 , issn =

    work page doi:10.1093/mnras/stx1616 2017

  15. [16]

    A first GLIMPSE into star clusters popula- tions across cosmic time

    2026 , author =. doi:10.48550/arXiv.2601.16281 , arxivId =

    work page doi:10.48550/arxiv.2601.16281 2026

  16. [17]

    Abbott, B. P. and Abbott, R. and Abbott, T. D. and Acernese, F. and Ackley, K. and Adams, C. and Adams, T. and Addesso, P. and Adhikari, R. X. and Adya, V. B. and Affeldt, C. and Afrough, M. and Agarwal, B. and Agathos, M. and Agatsuma, K. and Aggarwal, N. and Aguiar, O. D. and Aiello, L. and Ain, A. and Ajith, P. and Allen, B. and Allen, G. and Allocca, ...

    work page doi:10.1038/nature24471 2017

  17. [18]

    doi:10.1088/0067-0049/214/2/15 , arxivId =

    2014 , author =. doi:10.1088/0067-0049/214/2/15 , arxivId =

    work page doi:10.1088/0067-0049/214/2/15 2014

  18. [19]

    and Topping, Michael W

    Reddy, Naveen A. and Topping, Michael W. and Sanders, Ryan L. and Shapley, Alice E. and Brammer, Gabriel , number =. 2023 , journal =. doi:10.3847/1538-4357/acd754 , issn =

    work page doi:10.3847/1538-4357/acd754 2023

  19. [20]

    and Geach, James E

    Sobral, David and Smail, Ian and Best, Philip N. and Geach, James E. and Matsuda, Yuichi and Stott, John P. and Cirasuolo, Michele and Kurk, Jaron , number =. 2013 , journal =. doi:10.1093/MNRAS/STS096 , issn =

    work page doi:10.1093/mnras/sts096 2013

  20. [21]

    Khostovan, A. A. and Malhotra, S. and Rhoads, J. E. and Jiang, C. and Wang, J. and Wold, I. and Zheng, Z. Y. and Barrientos, L. F. and Coughlin, A. and Harish, S. and Hu, W. and Infante, L. and Perez, L. A. and Pharo, J. and Valdes, F. and Walker, A. R. and Yang, H. , number =. 2020 , booktitle =. doi:10.1093/mnras/staa175 , issn =

    work page doi:10.1093/mnras/staa175 2020

  21. [22]

    and Castellano, Marco and Akins, Hollis B

    Zavala, Jorge A. and Castellano, Marco and Akins, Hollis B. and Bakx, Tom J.L.C. and Burgarella, Denis and Casey, Caitlin M. and Ch. 2024 , journal =. doi:10.1038/S41550-024-02397-3 , issn =

    work page doi:10.1038/s41550-024-02397-3 2024

  22. [23]

    doi:10.1038/s41586-024-07191-9 , arxivId =

    2023 , author =. doi:10.1038/s41586-024-07191-9 , arxivId =

    work page doi:10.1038/s41586-024-07191-9 2023

  23. [24]

    2013, MNRAS, 436, 3031, doi: 10.1093/mnras/stt1789

    Vogelsberger, Mark and Genel, Shy and Sijacki, Debora and Torrey, Paul and Springel, Volker and Hernquist, Lars , month =. 2013 , journal =. doi:10.1093/mnras/stt1789 , arxivId =

    work page doi:10.1093/mnras/stt1789 2013

  24. [25]

    2023, MNRAS, 522, 3809, doi: 10.1093/mnras/stad1201

    Venditti, Alessandra and Graziani, Luca and Schneider, Raffaella and Pentericci, Laura and Di Cesare, Claudia and Maio, Umberto and Omukai, Kazuyuki , number =. 2023 , journal =. doi:10.1093/mnras/stad1201 , arxivId =

    work page doi:10.1093/mnras/stad1201 2023

  25. [26]

    , number =

    Hopkins, Philip F. , number =. 2015 , journal =. doi:10.1093/mnras/stv195 , issn =

    work page doi:10.1093/mnras/stv195 2015

  26. [27]

    and Katz, Harley and Rey, Martin P

    Cameron, Alex J. and Katz, Harley and Rey, Martin P. and Cameron, Alex J. and Katz, Harley and Rey, Martin P. , number =. 2023 , journal =

    2023

  27. [28]

    and Hernquist, Lars and Martini, Paul and Cox, Thomas J

    Hopkins, Philip F. and Hernquist, Lars and Martini, Paul and Cox, Thomas J. and Robertson, Brant and Di Matteo, Tiziana and Springel, Volker , number =. 2005 , journal =. doi:10.1086/431146 , issn =

    work page doi:10.1086/431146 2005

  28. [29]

    doi:10.3847/1538-4357/833/2/266 , arxivId =

    2016 , author =. doi:10.3847/1538-4357/833/2/266 , arxivId =

    work page doi:10.3847/1538-4357/833/2/266 2016

  29. [30]

    and Clayton, Geoffrey C

    Gordon, Karl D. and Clayton, Geoffrey C. and Misselt, K. A. and Landolt, Arlo U. and Wolff, Michael J. , number =. 2003 , journal =. doi:10.1086/376774 , arxivId =

    work page doi:10.1086/376774 2003

  30. [31]

    and Wilkinson, M

    Somerville, Rachel S. and Hopkins, Philip F. and Cox, Thomas J. and Robertson, Brant E. and Hernquist, Lars , number =. 2008 , journal =. doi:10.1111/j.1365-2966.2008.13805.x , issn =

    work page doi:10.1111/j.1365-2966.2008.13805.x 2008

  31. [32]

    doi:10.1093/mnras/stac3140 , arxivId =

    2022 , author =. doi:10.1093/mnras/stac3140 , arxivId =

    work page doi:10.1093/mnras/stac3140 2022

  32. [33]

    and Jones, A

    De Vis, P. and Jones, A. and Viaene, S. and Casasola, V. and Clark, C. J.R. and Baes, M. and Bianchi, S. and Cassara, L. P. and Davies, J. I. and De Looze, I. and Galametz, M. and Galliano, F. and Lianou, S. and Madden, S. and Manilla-Robles, A. and Mosenkov, A. V. and Nersesian, A. and Roychowdhury, S. and Xilouris, E. M. and Ysard, N. , month =. 2019 , ...

    work page doi:10.1051/0004-6361/201834444 2019

  33. [34]

    Nature Astronomy , keywords =

    Stein, Robert and Velzen, Sjoert van and Kowalski, Marek and Franckowiak, Anna and Gezari, Suvi and Miller-Jones, James C.A. and Frederick, Sara and Sfaradi, Itai and Bietenholz, Michael F. and Horesh, Assaf and Fender, Rob and Garrappa, Simone and Ahumada, Tomás and Andreoni, Igor and Belicki, Justin and Bellm, Eric C. and B. 2021 , journal =. doi:10.103...

    work page doi:10.1038/s41550-020-01295-8 2021

  34. [35]

    M.Diederik , number =

    Reina-Campos, Marta and Kruijssen, J. M.Diederik , number =. 2017 , journal =. doi:10.1093/MNRAS/STX790 , issn =

    work page doi:10.1093/mnras/stx790 2017

  35. [36]

    , number =

    Hasinger, G. , number =. 2008 , journal =. doi:10.1051/0004-6361:200809839 , issn =

    work page doi:10.1051/0004-6361:200809839 2008

  36. [37]

    and Sutherland, Ralph S

    Nicholls, David C. and Sutherland, Ralph S. and Dopita, Michael A. and Kewley, Lisa J. and Groves, Brent A. , number =. 2017 , journal =. doi:10.1093/mnras/stw3235 , issn =

    work page doi:10.1093/mnras/stw3235 2017

  37. [38]

    and Brinchmann, Jarle and Dickinson, Mark and Duc, Pierre Alain and Gobat, Raphael and Jean-Baptiste, Ingrid and Le Floc'H, Émeric and Lehnert, M

    Juneau, Stéphanie and Bournaud, Frédéric and Charlot, Stéphane and Daddi, Emanuele and Elbaz, David and Trump, Jonathan R. and Brinchmann, Jarle and Dickinson, Mark and Duc, Pierre Alain and Gobat, Raphael and Jean-Baptiste, Ingrid and Le Floc'H, Émeric and Lehnert, M. D. and Pacifici, Camilla and Pannella, Maurilio and Schreiber, Corentin , number =. 201...

    work page doi:10.1088/0004-637x/788/1/88 2014

  38. [39]

    and H., Julian , url =

    Krolik, Julian H. and H., Julian , url =. 1998 , journal =

    1998

  39. [40]

    and Springel, Volker and Li, Yuan and Burkhart, Blakesley and Choi, Ena and Faucher-Gigu

    Weinberger, Rainer and Su, Kung Yi and Ehlert, Kristian and Pfrommer, Christoph and Hernquist, Lars and Bryan, Greg L. and Springel, Volker and Li, Yuan and Burkhart, Blakesley and Choi, Ena and Faucher-Gigu. 2023 , journal =. doi:10.1093/mnras/stad1396 , issn =

    work page doi:10.1093/mnras/stad1396 2023

  40. [41]

    doi:10.3847/1538-4357/ada4a1 , issn =

    2025 , author =. doi:10.3847/1538-4357/ada4a1 , issn =

    work page doi:10.3847/1538-4357/ada4a1 2025

  41. [42]

    doi:10.1051/0004-6361/202449601 , arxivId =

    2024 , author =. doi:10.1051/0004-6361/202449601 , arxivId =

    work page doi:10.1051/0004-6361/202449601 2024

  42. [43]

    and Nagao, T

    Maiolino, R. and Nagao, T. and Grazian, A. and Cocchia, F. and Marconi, A. and Mannucci, F. and Cimatti, A. and Pipino, A. and Ballero, S. and Calura, F. and Chiappini, C. and Fontana, A. and Granato, L. and Matteucci, F. and Pastorini, G. and Pentericci, L. and Risaliti, G. and Salvati, M. and Silva, L. , number =. 2008 , journal =. doi:10.1051/0004-6361...

    work page doi:10.1051/0004-6361:200809678 2008

  43. [44]

    Kubo, Mariko and Umehata, Hideki and Matsuda, Yuichi and Kajisawa, Masaru and Steidel, Charles C. and Yamada, Toru and Tanaka, Ichi and Hatsukade, Bunyo and Tamura, Yoichi and Nakanishi, Kouichiro and Kohno, Kotaro and Lee, Kianhong and Matsuda, Keiichi and Ao, Yiping and Nagao, Tohru and Yun, Min S. , number =. 2022 , journal =. doi:10.3847/1538-4357/ac7...

    work page doi:10.3847/1538-4357/ac7f2d 2022

  44. [45]

    Fitzpatrick, E. L. and Massa, D. , number =. 2007 , journal =. doi:10.1086/518158/XML , issn =

    work page doi:10.1086/518158/xml 2007

  45. [46]

    doi:10.1093/mnras/staa3000 , arxivId =

    2020 , author =. doi:10.1093/mnras/staa3000 , arxivId =

    work page doi:10.1093/mnras/staa3000 2020

  46. [47]

    2018 , journal =

    Hernquist, Lars and Springel, Volker , number =. 2018 , journal =

    2018

  47. [48]

    and Copin, Y

    Hernquist, Lars and Springel, Volker , number =. 2003 , journal =. doi:10.1046/j.1365-8711.2003.06499.x , issn =

    work page doi:10.1046/j.1365-8711.2003.06499.x 2003

  48. [49]

    doi:10.3847/1538-4357/ad701c , arxivId =

    2023 , author =. doi:10.3847/1538-4357/ad701c , arxivId =

    work page doi:10.3847/1538-4357/ad701c 2023

  49. [50]

    and Vanzella, E

    De Barros, S. and Vanzella, E. and Amor. 2016 , journal =. doi:10.1051/0004-6361/201527046 , issn =

    work page doi:10.1051/0004-6361/201527046 2016

  50. [51]

    and Meyer, Romain A

    Covelo-Paz, Alba and Giovinazzo, Emma and Oesch, Pascal A. and Meyer, Romain A. and Weibel, Andrea and Brammer, Gabriel and Fudamoto, Yoshinobu and Kerutt, Josephine and Lin, Jamie and Matharu, Jasleen and Naidu, Rohan P. and Velichko, Anna and Bollo, Victoria and Bouwens, Rychard and Chisholm, John and Illingworth, Garth D. and Kramarenko, Ivan and Magee...

    work page doi:10.1051/0004-6361/202452363 2025

  51. [52]

    , number =

    Moustakas, John and Kennicutt, Jr., Robert C. , number =. 2006 , journal =. doi:10.1086/500971 , issn =

    work page doi:10.1086/500971 2006

  52. [53]

    Heckman, T. M. and. 1980 , journal =

    1980

  53. [54]

    Baroch, D. and Gim. 2021 , journal =. doi:10.1051/0004-6361/202040004 , issn =

    work page doi:10.1051/0004-6361/202040004 2021

  54. [55]

    and Loiacono, F

    Messa, Matteo and Vanzella, E. and Loiacono, F. and Bergamini, P. and Castellano, M. and Sun, B. and Willott, C. and Windhorst, R. A. and Yan, H. and Angora, G. and Rosati, P. and Adamo, A. and Annibali, F. and Bolamperti, A. and Brada. 2025 , journal =. doi:10.1051/0004-6361/202451695 , arxivId =

    work page doi:10.1051/0004-6361/202451695 2025

  55. [56]

    doi:10.1093/mnras/stad1225 , arxivId =

    2023 , author =. doi:10.1093/mnras/stad1225 , arxivId =

    work page doi:10.1093/mnras/stad1225 2023

  56. [57]

    M., & Gardner, J

    2023 , author =. doi:10.1093/mnras/stad3484 , arxivId =

    work page doi:10.1093/mnras/stad3484 2023

  57. [58]

    and Netzer, Hagai , month =

    Ferland, Gary J. and Netzer, Hagai , month =. 1983 , journal =. doi:10.1086/160577 , issn =

    work page doi:10.1086/160577 1983

  58. [59]

    2021, A&A, 649, A18, doi: 10.1051/0004-6361/202039701

    Galliano, Frédéric and Nersesian, Angelos and Bianchi, Simone and De Looze, Ilse and Roychowdhury, Sambit and Baes, Maarten and Casasola, Viviana and Cassar. 2021 , journal =. doi:10.1051/0004-6361/202039701 , keywords =

    work page doi:10.1051/0004-6361/202039701 2021

  59. [60]

    2020 , journal =

    Carraro, R and Rodighiero, G and Cassata, P and Brusa, M and Shankar, F and Baronchelli, I and Daddi, E and Delvecchio, I and Franceschini, A and Griffiths, R and Gruppioni, C and L. 2020 , journal =. doi:10.1051/0004-6361/201936649 , keywords =

    work page doi:10.1051/0004-6361/201936649 2020

  60. [61]

    2009 , journal =

    Paradis, D and Bernard, J.-Ph and M. 2009 , journal =. doi:10.1051/0004-6361/200811246 , keywords =

    work page doi:10.1051/0004-6361/200811246 2009

  61. [62]

    2017 , journal =

    Wiseman, P and Schady, P and Bolmer, J and Kr. 2017 , journal =. doi:10.1051/0004-6361/201629228 , keywords =

    work page doi:10.1051/0004-6361/201629228 2017

  62. [63]

    2017 , journal =

    Chastenet, Jérémy and Bot, Caroline and Gordon, Karl D and Bocchio, Marco and Roman-Duval, Julia and Jones, Anthony P and Ysard, Nathalie , pages =. 2017 , journal =. doi:10.1051/0004-6361/201629133 , keywords =

    work page doi:10.1051/0004-6361/201629133 2017

  63. [64]

    and Ferland, Gary J

    Osterbrock, Donald E. and Ferland, Gary J. , publisher =. 2006 , booktitle =

    2006

  64. [65]

    doi:10.1093/mnras/stad2267 , arxivId =

    2023 , author =. doi:10.1093/mnras/stad2267 , arxivId =

    work page doi:10.1093/mnras/stad2267 2023

  65. [66]

    and Schaye, Joop , month =

    Mitchell, Peter D. and Schaye, Joop , month =. 2021 , journal =. doi:10.1093/mnras/stab3686 , arxivId =

    work page doi:10.1093/mnras/stab3686 2021

  66. [67]

    doi:10.48550/arXiv.1810.01883 , keywords =

    2019 , author =. doi:10.48550/arXiv.1810.01883 , keywords =

    work page doi:10.48550/arxiv.1810.01883 2019

  67. [68]

    and Bryan, Greg L

    Dave, Romeel and Cen, Renyue and Ostriker, Jeremiah P. and Bryan, Greg L. and Hernquist, Lars and Katz, Neal and Weinberg, David H. and Norman, Michael L. and O’Shea, Brian , number =. 2001 , journal =. doi:10.1086/320548 , issn =

    work page doi:10.1086/320548 2001

  68. [69]

    2022 , journal =

    Vidal-Garc. 2022 , journal =

    2022

  69. [70]

    Concas, Alice and Maiolino, Roberto and Curti, Mirko and Hayden-Pawson, Connor and Cirasuolo, Michele and Jones, Gareth C. and Mercurio, Amata and Belfiore, Francesco and Cresci, Giovanni and Cullen, Fergus and Mannucci, Filippo and Marconi, Alessandro and Cappellari, Michele and Cicone, Claudia and Peng, Yingjie and Troncoso, Paulina , number =. 2022 , j...

    work page doi:10.1093/mnras/stac1026 2022

  70. [71]

    2024 , journal =

    Roberts-Borsani, Guido and Treu, Tommaso and Shapley, Alice and Fontana, Adriano and Pentericci, Laura and Castellano, Marco and Morishita, Takahiro and Bergamini, Pietro and Rosati, Piero , number =. 2024 , journal =. doi:10.3847/1538-4357/ad85d3 , issn =

    work page doi:10.3847/1538-4357/ad85d3 2024

  71. [72]

    2005 , journal =

    Stasi. 2005 , journal =. doi:10.1051/0004-6361:20042216 , issn =

    work page doi:10.1051/0004-6361:20042216 2005

  72. [73]

    L., Shapley, A

    Sanders, Ryan L. and Shapley, Alice E. and Zhang, Kai and Yan, Renbin , number =. 2017 , journal =. doi:10.3847/1538-4357/aa93e4 , issn =

    work page doi:10.3847/1538-4357/aa93e4 2017

  73. [75]

    Eldridge, J. J. and Stanway, E. R. and Xiao, L. and McClelland, L. A.S. and Taylor, G. and Ng, M. and Greis, S. M.L. and Bray, J. C. , pages =. 2017 , journal =. doi:10.1017/pasa.2017.51 , issn =

    work page Pith review doi:10.1017/pasa.2017.51 2017

  74. [76]

    2019 , journal =

    Thomas, Nicole and Dav. 2019 , journal =. doi:10.1093/mnras/stz1703 , arxivId =

    work page doi:10.1093/mnras/stz1703 2019

  75. [77]

    and Vanzella, Eros and Claeyssens, Adélaïde and Welch, Brian and Diego, Jose M

    Adamo, Angela and Bradley, Larry D. and Vanzella, Eros and Claeyssens, Adélaïde and Welch, Brian and Diego, Jose M. and Mahler, Guillaume and Oguri, Masamune and Sharon, Keren and. 2024 , journal =. doi:10.1038/s41586-024-07703-7 , issn =

    work page doi:10.1038/s41586-024-07703-7 2024

  76. [78]

    Murphy, E. J. and Condon, J. J. and Schinnerer, E. and Kennicutt, R. C. and Calzetti, D. and Armus, L. and Helou, G. and Turner, J. L. and Aniano, G. and Beir. 2011 , journal =. doi:10.1088/0004-637X/737/2/67 , issn =

    work page doi:10.1088/0004-637x/737/2/67 2011

  77. [79]

    and Treu, T

    Nipoti, C. and Treu, T. and Auger, M. W. and Bolton, A. S. , number =. 2009 , journal =. doi:10.1088/0004-637X/706/1/L86 , issn =

    work page doi:10.1088/0004-637x/706/1/l86 2009

  78. [80]

    Baugh, C. M. and Lacey, C. G. and Frenk, C. S. and Granato, G. L. and Silva, L. and Bressan, A. and Benson, A. J. and Cole, S. and Baugh, C. M. and Lacey, C. G. and Frenk, C. S. and Granato, G. L. and Silva, L. and Bressan, A. and Benson, A. J. and Cole, S. , number =. 2005 , journal =. doi:10.1111/J.1365-2966.2004.08553.X , issn =

    work page doi:10.1111/j.1365-2966.2004.08553.x 2005

  79. [81]

    doi:10.1093/mnras/stad3374 , arxivId =

    2023 , author =. doi:10.1093/mnras/stad3374 , arxivId =

    work page doi:10.1093/mnras/stad3374 2023

  80. [82]

    and Garc

    Esteban, C. and Garc. 2014 , journal =. doi:10.1093/MNRAS/STU1177 , issn =

    work page doi:10.1093/mnras/stu1177 2014

Showing first 80 references.