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The Thesan-Zoom project: bursty star formation is incompatible with prolonged dust survival

T0 review · 3 major / 5 minor · reviewed 2026-07-13 · grok-4.5

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Pith's one-line read Bursty star formation prevents large dust reservoirs from lasting long in early galaxies.

desk verdict Solid dust analysis of Thesan-Zoom that cleanly shows, inside this model, bursty SF cannot keep large dust reservoirs; the UVLF implication is real but rests on missing dense-clump shielding. read the letter →

arxiv 2607.08824 v1 pith:K64V5BKH submitted 2026-07-09 astro-ph.GA

Enrico Garaldi , Filip Popovic , Rahul Kannan , Aaron Smith , Ewald Puchwein , Naoki Yoshida , Kentaro Nagamine , Celine Peroux
show 6 more authors
Laura Keating Mark Vogelsberger William McClymont Xuejian Shen Sandro Tacchella Lars Hernquist
This is my paper
classification astro-ph.GA
keywords cosmicdustburstystarformationhigh-redshiftgalaxiessurvivalUVattenuationthesan-zoomISMfeedbacktemperature
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper argues that, in a self-consistent radiation-hydrodynamical model of early galaxies, short intense star-formation bursts repeatedly destroy and eject dust so thoroughly that large dust reservoirs cannot persist for most of cosmic time. The simulated systems match several observed dust-to-gas and dust-to-metal trends and produce realistic dust temperatures and UV–IR spatial offsets during brief IR-bright windows, yet they under-produce UV attenuation and dust mass at high specific star-formation rates. The central claim is therefore that burstiness and prolonged dust survival are incompatible inside this framework. That incompatibility matters because bursty star formation is frequently invoked to explain the excess of UV-bright galaxies seen at redshift greater than or equal to 10: if the same burstiness also erases dust, the bursts must settle by redshift approximately 8, where substantial dust is already observed, or else missing physics must protect dust from feedback.

What carries the argument

The coupled on-the-fly dust model (formation via stellar yields, metallicity-dependent accretion, thermal and supernova sputtering) fully linked to multi-phase ISM and SMUGGLE stellar feedback; the machinery shows that feedback co-spatial with newly formed dust preferentially destroys and ejects it after each burst.

What would settle it

Deep continuum or absorption measurements showing large dust reservoirs (M_dust/M_star greater than or equal to 10^{-3}) coexisting with high specific star-formation rates in a statistical sample of z greater than or equal to 10 UV-bright galaxies would falsify the claimed incompatibility.

Watch

Extended reading notes

Core claim

In the thesan-zoom model, bursty star formation prevents large dust reservoirs (M_dust/M_star greater than or equal to 10^{-3}) from surviving over a significant fraction of cosmic time; short-lived IR-bright phases (median duration roughly 20 Myr) alternate with longer dust-poor phases, so that observed dust properties and the high-redshift UV luminosity function can be reconciled only if burstiness declines rapidly by z approximately 8 or if additional shielding physics is present.

Load-bearing premise

The assumption that the adopted sub-grid dust physics and feedback scheme correctly capture how dust survives, even though unresolved dense clumps that could shield dust are missing.

Editorial extensions

If this is right

  • Bursty star formation can explain the z greater than or equal to 10 UV-bright excess only if it rapidly settles by z approximately 8, where large dust reservoirs are already detected.
  • Observed IR-bright high-redshift galaxies are short-lived post-burst phases lasting only tens of Myr and are therefore biased relative to the bulk population.
  • Dust-poor post-starburst phases should preferentially allow high escape fractions of ionizing photons.
  • A mechanism that shields dust from strong feedback is required if the same galaxy-formation model is to match the higher observed UV attenuation at lower redshifts.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If unresolved cold clumps systematically protect dust, models that currently under-produce attenuation may still be viable once resolution or sub-grid shielding improves.
  • A statistical sample of dust masses in UV-selected z greater than 10 galaxies would cleanly discriminate between pure burstiness and models that retain dust while still producing UV variability.
  • The same cycle that erases dust after each burst may also explain why some high-redshift samples appear split into dust-rich and dust-poor populations without requiring two distinct formation channels.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 5 minor

Summary. The paper analyses cosmic dust in the Thesan-Zoom radiation-hydrodynamical zoom-in suite, which couples an on-the-fly dust model (adapted from McKinnon et al. 2016, 2017) to multi-phase ISM physics, SMUGGLE feedback and radiative transfer at z ≥ 3. Simulated galaxies reproduce observed DGR and DMR trends with metallicity and broadly match dust temperatures and UV–IR offsets, but show a dust deficit at high sSFR and systematically low A1500 even after TODDLERS post-processing of unresolved birth-cloud dust. The central claim is that the emergent bursty star-formation cycle (illustrated in Sec. 5.1 and Fig. 15) produces short-lived IR-bright phases (median ~20 Myr) and longer dust-poor phases, so that large reservoirs (M_dust/M_star ≳ 10^{-3}) cannot survive for a significant fraction of cosmic time; therefore bursty SF can explain the z ≳ 10 UVLF excess only if it settles by z ~ 8, or the model is missing shielding physics.

Significance. If the result holds, it supplies a concrete, falsifiable constraint linking two major high-z puzzles: the JWST UVLF excess and the presence of substantial dust reservoirs by z ~ 8. The work is valuable because it is one of the few suites that self-consistently couples live dust, multi-phase ISM and radiation, produces quantitative predictions (IR-phase duty cycle, T_dust–ΔMS correlation, UV–IR offsets) that can be tested with ALMA/NOEMA and JWST, and explicitly flags the model limitations that would reverse the conclusion. The forward-modelling of UV–IR offsets and dust surface-density distributions, and the transparent comparison to multiple observational samples and other simulations, are clear strengths.

major comments (3)
  1. Sec. 5.1 and Fig. 15 establish the co-spatial growth–destruction cycle that underpins the incompatibility claim, yet Sec. 2.2, Sec. 5.4 and Appendix B acknowledge that unresolved cold dense clumps (n ≳ 10 cm^{-3}, T ≲ 100 K) capable of shielding dust from the SMUGGLE injection kernel are missing. Because the paper itself identifies this as the softest link, the central statement that bursty SF is incompatible with prolonged survival of M_dust/M_star ≳ 10^{-3} should be explicitly conditioned on the absence of such shielding, and a quantitative estimate (or at least a clear statement of the required change in destruction efficiency or recovery timescale) should be added so that the UVLF implication remains falsifiable rather than model-contingent.
  2. Sec. 4.3 and Fig. 14 show that A1500 remains low compared with observations even after TODDLERS birth-cloud dust is included. The abstract and Sec. 5 correctly note that a shielding mechanism is therefore required, but the paper does not quantify how much additional shielded dust (or what change in feedback topology) would be needed to reach the observed A1500 while preserving the bursty UVLF success at z ≳ 10. Without that estimate the claim that the model is already close enough for the duty-cycle argument to be robust is under-supported.
  3. The single effective grain size a_eff = 0.1 μm and the restriction of accretion to star-forming gas (Eq. 1 and Sec. 2.2) lock dust production to the same dense gas that later hosts feedback. Sec. 5.4 mentions grain-size evolution only in passing. A short test or literature-based estimate of how a multi-bin size distribution (or accretion outside star-forming gas) would alter the post-burst recovery timescale would strengthen the claim that the incompatibility is robust to dust-physics uncertainties.
minor comments (5)
  1. Fig. 2 caption and text: the vertical stripes of constant M_star are attributed to rapid dust growth; a brief note that they could also reflect temporary dust ejection followed by re-accretion would avoid over-interpretation.
  2. Sec. 3.6: the statement that dust temperatures >100 K 'should be easily observable but have not been detected' needs a short caveat on the limited volume and mass range of the zoom sample.
  3. Eq. (1): the ad-hoc assignment of T = 10^4 K to star-forming gas for the accretion timescale is tested in Appendix B, but the main text should flag this assumption more prominently when the growth rate is first introduced.
  4. Fig. 12: the assumed Gaussian PSF with σ = 0.5 pkpc is reasonable for a population comparison, but a sentence noting the range of actual ALMA beams in the REBELS/ALPINE samples would help readers judge the comparison.
  5. Throughout: a few typographical inconsistencies remain (e.g., 'thesan-zoom' capitalisation, occasional missing spaces around Å). A light copy-edit pass would improve readability.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: the incompatibility claim is an emergent simulation outcome compared to external data, not a definitional or fitted reduction.

full rationale

The paper's central claim—that bursty star formation prevents prolonged survival of large dust reservoirs (M_dust/M_star ≳ 10^{-3})—is obtained by running thesan-zoom (SMUGGLE feedback + McKinnon-style dust) and inspecting the resulting time series (Fig. 15, Sec. 5.1). Dust growth, sputtering, and ejection are computed from the stated sub-grid equations (Eqs. 1–3); burstiness is an emergent property already documented in companion papers, not redefined here to force the dust result. Scaling relations and attenuation are then compared to independent ALMA/JWST/DLA observations. The dust model is taken from McKinnon et al. (2016, 2017) with modest updates (metallicity dependence, T_gas threshold); those citations are external and do not encode the high-z UVLF implication. No equation equates a fitted parameter to a claimed prediction by construction, and no uniqueness theorem is imported from the authors to forbid alternatives. The softest link is physical (missing dense-clump shielding, single grain size), which is a model-limitation issue, not circularity. Score 1 for ordinary self-citation of the simulation suite and dust module; the derivation chain itself is self-contained against external benchmarks.

Assumptions & free parameters 4 free parameters · 4 assumptions · 0 invented entities

Central claim rests on the McKinnon-style dust sub-grid model (single grain size, accretion only in star-forming gas, SN + thermal sputtering) coupled to SMUGGLE feedback that produces the bursty SFHs. Free parameters are those inherited or lightly retuned from the original dust model; no new particles or forces are invented. Domain assumptions about multi-phase ISM resolution and CMB optical thinness are stated.

free parameters (4)
  • a_eff (effective grain size) = 0.1 μm
    Fixed at 0.1 μm; controls accretion and sputtering timescales (Eq. 1–3). Chosen as representative of AGB/SN grains; total dust mass only weakly sensitive per McKinnon et al. Appendix B.
  • τ_growth normalisation and Z dependence = 3 Gyr (at n=100 cm^{-3}, T=20 K, Z=Z_⊙)
    3 Gyr base timescale with extra Z_⊙/Z_gas factor (Eq. 1); metallicity dependence newly added relative to original McKinnon model.
  • T_gas,thr for accretion = 300 K
    New 300 K temperature ceiling for growth; ad-hoc addition to suppress accretion at high relative velocities.
  • SN grain destruction efficiency ε
    Inherited from McKinnon et al.; multiplies local SN rate in sputtering timescale.
assumptions (4)
  • domain assumption Dust is a passive scalar advected with gas (no dust–gas drag).
    Sec. 2.2; standard approximation at the densities resolved here.
  • ad hoc to paper Star-forming gas is assigned fixed T=10^4 K only for the accretion timescale calculation.
    Sec. 2.2; formally inconsistent with the 300 K threshold but shown in Appendix B to have negligible effect.
  • domain assumption CMB is optically thin to the relevant photons, so dust cannot cool below T_CMB.
    Sec. 2.2; authors note possible breakdown only in extreme n≳10^6 cm^{-3}, Z≳Z_⊙ regions.
  • domain assumption SMUGGLE stellar feedback produces realistic bursty SFHs that match the z≳10 UVLF.
    Sec. 2.1 and McClymont et al. 2025a; load-bearing for the incompatibility claim.

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Cite this review

Pith. "Pith review of The Thesan-Zoom project: bursty star formation is incompatible with prolonged dust survival." pith.science (2026). https://pith.science/paper/K64V5BKH

@misc{pith2026260708824,
  author       = {Pith},
  title        = {Pith review of: The Thesan-Zoom project: bursty star formation is incompatible with prolonged dust survival},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/K64V5BKH}},
  note         = {Machine review of arXiv:2607.08824}
}
abstract

Cosmic dust is a key regulator of galaxy evolution, but its build-up and survival in the first billion years remain poorly constrained. We present a systematic analysis of dust in the thesan-zoom suite of radiation-hydrodynamical zoom-in simulations, which self-consistently model dust formation, growth, destruction, and its coupling to radiative transfer in galaxies at $z \geq 3$, a multi-phase ISM and bursty star formation histories. The simulated galaxies reproduce the observed trends of dust-to-gas and dust-to-metal ratios with gas metallicity, while showing a dust deficit at high specific star-formation rates. They also broadly match observed dust temperatures and UV-IR spatial offsets. We find that dust and its properties are strongly time-variable and tightly linked to bursty star formation, with short-lived IR-bright phases (median duration of $20.3^{+2.3}_{-2.4}$ Myr) and longer dust-poor phases, naturally producing a correlation between dust temperature and distance from the star-forming main sequence. The predicted attenuation at $1500$ \r{A} is low compared to observations, even when including unresolved dust through post processing, indicating that a mechanism able to shield dust from strong feedback events is necessary to reconcile our galaxy formation model with observations. In our model, bursty star formation prevents the survival of large dust reservoirs ($M_{dust} / M_{star} \geq 10^{-3}$) over a significant fraction of cosmic time. This implies that bursty star formation can produce the observed overabundance of UV-bright galaxies at $z \geq 10$ only if it rapidly settles down by $z \sim 8$ (where large dust reservoirs are detected). It is also possible that our models lack physical ingredients or emergent phenomena that aid the survival of dust. Future observations of high-redshift dust will be key to diagnose the physical mechanism at play in the first galaxies.

Figures

Figures reproduced from arXiv: 2607.08824 by the authors.

Figure 1
Figure 1. — Overview of dust-related properties in two thesan-zoom galaxies. The vertical sequences on the left and right of the plot show the evolution of the projected stellar mass content in the m11.9 (left) and m12.6 (right) haloes. The size of the panel is set to 140 comoving kpc/ℎ. In the middle part of the Figure, we show two sets of plots (the halo depicted and the redshift are reported in the top left corner). The pa… view at source ↗
Figure 2
Figure 2. — Dust-to-stellar mass relation for thesan-zoom galaxies. Each row shows a different redshift range. Panels on the right side show zoom-ins of the high Mstar end, with the vertical axis normalized by Mstar for visual clarity. Different colored symbols represent different targets and resolution levels. The gray background histogram shows simulated all-HR. Dark grey symbols report individual observations from da Cunha… view at source ↗
Figure 3
Figure 3. — [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figures from the paper (11 more)
Figure 4
Figure 4. Figure 4: — Dust mass function estimated from thesan-zoom (see text for details on how it is computed) over the redshift range 3 ≤ 𝑧 ≤ 15 (colored solid lines), compared to models from Popping et al. (2017, dotted orange line), Lewis et al. (2023, long-dashed green line), Grazia…
Figure 5
Figure 5. Figure 5: — Dust-to-gas mass ratio (DGR) as a function of gas-phase metallicity for thesan-zoom galaxies. Each panel shows a different redshift range. Different colors represent different targets while symbols reflect their resolution level. The gray background histogram shows n…
Figure 6
Figure 6. Figure 6: — Dust-to-metal ratio (DMR) as function of gas-phase metallicity (𝑍gas) for thesan-zoom galaxies. The DMR is normalized by the Milky Way value (DMRMW = 0.44). Each panel shows a different redshift range. Colors represent different targets while symbols reflect their re…
Figure 7
Figure 7. Figure 7: — Dust temperature evolution in thesan-zoom. Target galaxies are shown using colored lines, while other high-resolution galaxies identi￾fied at 𝑧 = 3 are shown in grey. The red histogram shows the average dust temperature and its standard deviation (shaded region) comp…
Figure 9
Figure 9. Figure 9: — Radial dust density profile at 𝑧 = 3 for thesan-zoom targets (colored lines) and all-HR (grey thin lines, their median profile is indicated by a dark grey dashed line). Different zoom factors are reported with different line styles, as indicated in the legend. The ra…
Figure 10
Figure 10. Figure 10: —Dust-to-gas (top) and gas-to-stellar (bottom) size evolution. All radii are computed as twice the half-mass radius of the component, while the thick black lines show their median. Thin lines show the value for individual thesan-zoom targets, with different line style…
Figure 11
Figure 11. Figure 11: —Examples of UV–IR offsets(or lack thereof) in simulated galaxies at 𝑧 = 6. Each 3-panel collage refers to a different redshift (reported on the left) and galaxy (reported on the top left, followed by the zoom level). Within each collage, the left and central panels s…
Figure 12
Figure 12. Figure 12: — UV–IR spatial offsets as function of stellar mass (left) and specific star formation rate (right). The median for thesan-zoom galaxies in three redshift bins (red, green and yellow histograms, see legend) is shown using a solid histogram, while the central 68% of th…
Figure 13
Figure 13. Figure 13: — Dust surface density distribution function 𝑓 (Σdust) in thesan￾zoom galaxies at 𝑧 = 6. Light-grey violins show the distribution from 104 random sampling of sightlines through each of the target galaxies, while the red violin shows the distribution of the full sample…
Figure 14
Figure 14. Figure 14: — Attenuation at 1500 Å as a function of stellar mass in the thesan-zoom galaxies, augmented with the TODDLERS model for unre￾solved dust in the stellar birth cloud. The colored symbols show the target galaxies (using circles, squares and diamonds for zoom factor 4, 8…
Figure 15
Figure 15. Figure 15: — Time evolution of physical properties of three sample thesan-zoom galaxies, namely the m12.2z4, m11.5z4 and m10.4z8 runs (left to right column, respectively). From top to bottom, we show with coloured thick lines the dust-to-total-mass ratio, gas-to-total-mass ratio…

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Reference graph

Works this paper leans on

226 extracted references · 7 canonical work pages · cited by 1 Pith paper

  1. [1]

    J., et al., 2023, @doi [ ] 10.1093/mnras/stac3347 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.518.4755A 518, 4755

    Adams N. J., et al., 2023, @doi [ ] 10.1093/mnras/stac3347 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.518.4755A 518, 4755

    doi:10.1093/mnras/stac3347 2023

  2. [2]

    B., et al., 2022, @doi [ ] 10.3847/1538-4357/ac795b , https://ui.adsabs.harvard.edu/abs/2022ApJ...934...64A 934, 64

    Akins H. B., et al., 2022, @doi [ ] 10.3847/1538-4357/ac795b , https://ui.adsabs.harvard.edu/abs/2022ApJ...934...64A 934, 64

    doi:10.3847/1538-4357/ac795b 2022

  3. [3]

    Algera H. S. B., et al., 2023, @doi [ ] 10.1093/mnras/stac3195 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.518.6142A 518, 6142

    doi:10.1093/mnras/stac3195 2023

  4. [4]

    Algera H. S. B., et al., 2024, @doi [ ] 10.1093/mnras/stae1994 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.533.3098A 533, 3098

    doi:10.1093/mnras/stae1994 2024

  5. [5]

    Algera H. S. B., et al., 2026, @doi [ ] 10.1093/mnras/staf1897 , https://ui.adsabs.harvard.edu/abs/2026MNRAS.545f1897A 545, staf1897

    doi:10.1093/mnras/staf1897 2026

  6. [6]

    Aoyama S., Hou K.-C., Shimizu I., Hirashita H., Todoroki K., Choi J.-H., Nagamine K., 2016, @doi [ ] 10.1093/mnras/stw3061 , 466, 105

    doi:10.1093/mnras/stw3061 2016

  7. [7]

    Aoyama S., Hou K.-C., Hirashita H., Nagamine K., Shimizu I., 2018, @doi [ ] 10.1093/mnras/sty1431 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.478.4905A 478, 4905

    doi:10.1093/mnras/sty1431 2018

  8. [8]

    Aoyama S., Hirashita H., Nagamine K., 2020, @doi [ ] 10.1093/mnras/stz3253 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.491.3844A 491, 3844

    doi:10.1093/mnras/stz3253 2020

Show all 226 references
  1. [9]

    Arrabal Haro P., et al., 2023, @doi [ ] 10.3847/2041-8213/acdd54 , https://ui.adsabs.harvard.edu/abs/2023ApJ...951L..22A 951, L22

    2023 doi

  2. [10]

    Atek H., et al., 2023, @doi [ ] 10.1093/mnras/stac3144 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.519.1201A 519, 1201

    2023 doi

  3. [11]

    M., et al., 2025, @doi [ ] 10.1051/0004-6361/202557207 , 706, A91

    Baker W. M., et al., 2025, @doi [ ] 10.1051/0004-6361/202557207 , 706, A91

    2025 doi

  4. [12]

    Bakx T. J. L. C., et al., 2021, @doi [ ] 10.1093/mnrasl/slab104 , 508, L58

    2021 doi

  5. [13]

    Bakx T. J. L. C., et al., 2024a, @doi [ ] 10.1093/mnras/stae1613 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.532.2270B 532, 2270

    doi

  6. [14]

    Bakx T. J. L. C., et al., 2024b, @doi [ ] 10.1093/mnras/stae2409 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.535.1533B 535, 1533

    doi

  7. [15]

    Bakx T. J. L. C., et al., 2025, @doi [ ] 10.1093/mnras/staf1714 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.544.1502B 544, 1502

    2025 doi

  8. [16]

    Bakx T. J. L. C., et al., 2026, @doi [ ] 10.1093/mnras/staf2284 , https://ui.adsabs.harvard.edu/abs/2026MNRAS.546f2284B 546, staf2284

    2026 doi

  9. [17]

    S., Wechsler R

    Behroozi P. S., Wechsler R. H., Conroy C., 2013, @doi [ ] 10.1088/0004-637X/770/1/57 , https://ui.adsabs.harvard.edu/abs/2013ApJ...770...57B 770, 57

    2013 doi

  10. [18]

    Bekki K., 2013, @doi [ ] 10.1093/mnras/stt589 , 432, 2298

    2013 doi

  11. [19]

    Bekki K., 2015, @doi [ ] 10.1088/0004-637X/799/2/166 , https://ui.adsabs.harvard.edu/abs/2015ApJ...799..166B 799, 166

    2015 doi

  12. [20]

    B \'e thermin M., et al., 2015, @doi [ ] 10.1051/0004-6361/201425031 , https://ui.adsabs.harvard.edu/abs/2015A&A...573A.113B 573, A113

    2015 doi

  13. [21]

    B \'e thermin M., et al., 2020, @doi [ ] 10.1051/0004-6361/202037649 , https://ui.adsabs.harvard.edu/abs/2020A&A...643A...2B 643, A2

    2020 doi

  14. [22]

    Bhagwat A., Costa T., Ciardi B., Pakmor R., Garaldi E., 2024, @doi [ ] 10.1093/mnras/stae1125 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.531.3406B 531, 3406

    2024 doi

  15. [23]

    Bianchi S., Schneider R., 2007, @doi [ ] 10.1111/j.1365-2966.2007.11829.x , https://ui.adsabs.harvard.edu/abs/2007MNRAS.378..973B 378, 973

    2007 doi

  16. [24]

    Boquien M., et al., 2022, @doi [ ] 10.1051/0004-6361/202142537 , https://ui.adsabs.harvard.edu/abs/2022A&A...663A..50B 663, A50

    2022 doi

  17. [25]

    stad2523

    Borrow J., Kannan R., Garaldi E., Smith A., Vogelsberger M., Pakmor R., Springel V., Hernquist L., 2023, @doi [ ] 10.1093/mnras/stad2523 , p. stad2523

    2023 doi

  18. [26]

    J., et al., 2022, @doi [ ] 10.3847/1538-4357/ac5a4a , https://ui.adsabs.harvard.edu/abs/2022ApJ...931..160B 931, 160

    Bouwens R. J., et al., 2022, @doi [ ] 10.3847/1538-4357/ac5a4a , https://ui.adsabs.harvard.edu/abs/2022ApJ...931..160B 931, 160

    2022 doi

  19. [27]

    Bouwens R., Illingworth G., Oesch P., Stefanon M., Naidu R., van Leeuwen I., Magee D., 2023, @doi [ ] 10.1093/mnras/stad1014 , 523, 1009

    2023 doi

  20. [28]

    Bowler R. A. A., Cullen F., McLure R. J., Dunlop J. S., Avison A., 2022, @doi [ ] 10.1093/mnras/stab3744 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.510.5088B 510, 5088

    2022 doi

  21. [29]

    D., et al., 2008, @doi [ ] 10.1086/533519 , 678, 647

    Bradley L. D., et al., 2008, @doi [ ] 10.1086/533519 , 678, 647

    2008 doi

  22. [30]

    J., et al., 2023, @doi [ ] 10.1051/0004-6361/202346159 , https://ui.adsabs.harvard.edu/abs/2023A&A...677A..88B 677, A88

    Bunker A. J., et al., 2023, @doi [ ] 10.1051/0004-6361/202346159 , https://ui.adsabs.harvard.edu/abs/2023A&A...677A..88B 677, A88

    2023 doi

  23. [31]

    K., Takeuchi T

    Burgarella D., Nanni A., Hirashita H., Theul \'e P., Inoue A. K., Takeuchi T. T., 2020, @doi [ ] 10.1051/0004-6361/201937143 , https://ui.adsabs.harvard.edu/abs/2020A&A...637A..32B 637, A32

    2020 doi

  24. [32]

    Burgarella D., et al., 2025, @doi [ ] 10.1051/0004-6361/202554231 , https://ui.adsabs.harvard.edu/abs/2025A&A...699A.336B 699, A336

    2025 doi

  25. [33]

    arXiv:2605.09829

    Burgarella D., et al., 2026, @doi [arXiv e-prints] 10.48550/arXiv.2605.09829 , https://ui.adsabs.harvard.edu/abs/2026arXiv260509829B p. arXiv:2605.09829

    2026 doi arXiv

  26. [34]

    Camps P., Baes M., 2020, @doi [Astronomy and Computing] 10.1016/j.ascom.2020.100381 , https://ui.adsabs.harvard.edu/abs/2020A&C....3100381C 31, 100381

    2020 doi

  27. [35]

    Carniani S., et al., 2024, @doi [ ] 10.1038/s41586-024-07860-9 , https://ui.adsabs.harvard.edu/abs/2024Natur.633..318C 633, 318

    2024 doi

  28. [36]

    Castellano M., et al., 2022, @doi [ ] 10.3847/2041-8213/ac94d0 , https://ui.adsabs.harvard.edu/abs/2022ApJ...938L..15C 938, L15

    2022 doi

  29. [37]

    Castellano M., et al., 2024, @doi [ ] 10.3847/1538-4357/ad5f88 , https://ui.adsabs.harvard.edu/abs/2024ApJ...972..143C 972, 143

    2024 doi

  30. [38]

    Cazaux S., Tielens A. G. G. M., 2002, @doi [ ] 10.1086/342607 , https://ui.adsabs.harvard.edu/abs/2002ApJ...575L..29C 575, L29

    2002 doi

  31. [39]

    Cazaux S., Tielens A. G. G. M., 2004, @doi [ ] 10.1086/381775 , https://ui.adsabs.harvard.edu/abs/2004ApJ...604..222C 604, 222

    2004 doi

  32. [40]

    Ceverino D., Glover S. C. O., Klessen R. S., 2017, @doi [ ] 10.1093/mnras/stx1386 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.470.2791C 470, 2791

    2017 doi

  33. [41]

    Ceverino D., et al., 2024, @doi [ ] 10.1093/mnras/stad3332 , 527, 2139

    2024 doi

  34. [42]

    Chemerynska I., et al., 2024, @doi [ ] 10.1093/mnras/stae1260 , 531, 2615

    2024 doi

  35. [43]

    Chisholm J., et al., 2018, @doi [ ] 10.1051/0004-6361/201832758 , https://ui.adsabs.harvard.edu/abs/2018A&A...616A..30C 616, A30

    2018 doi

  36. [44]

    Chisholm J., et al., 2022, @doi [ ] 10.1093/mnras/stac2874 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.517.5104C 517, 5104

    2022 doi

  37. [45]

    R., Kereš D., Hopkins P

    Choban C. R., Kereš D., Hopkins P. F., Sandstrom K. M., Hayward C. C., Faucher-Giguère C.-A., 2022, @doi [ ] 10.1093/mnras/stac1542 , 514, 4506

    2022 doi

  38. [46]

    R., Salim S., Kere s D., Hayward C

    Choban C. R., Salim S., Kere s D., Hayward C. C., Sandstrom K. M., 2025, @doi [ ] 10.1093/mnras/staf118 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.537.1518C 537, 1518

    2025 doi

  39. [47]

    R., Salim S., Kere s D., Roman-Duval J., Sandstrom K

    Choban C. R., Salim S., Kere s D., Roman-Duval J., Sandstrom K. M., 2026, @doi [arXiv e-prints] 10.48550/arXiv.2603.08504 , https://ui.adsabs.harvard.edu/abs/2026arXiv260308504C p. arXiv:2603.08504

    2026 doi arXiv

  40. [48]

    S., et al., 2013, @doi [ ] 10.1093/mnras/stt760 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.433..695C 433, 695

    Clemens M. S., et al., 2013, @doi [ ] 10.1093/mnras/stt760 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.433..695C 433, 695

    2013 doi

  41. [49]

    Curtis-Lake E., et al., 2023, @doi [Nature Astronomy] 10.1038/s41550-023-01918-w , https://ui.adsabs.harvard.edu/abs/2023NatAs.tmp...66C

    2023 doi

  42. [50]

    Dayal P., et al., 2022, @doi [ ] 10.1093/mnras/stac537 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.512..989D 512, 989

    2022 doi

  43. [51]

    B., 2016, @doi [ ] 10.1051/0004-6361/201527895 , https://ui.adsabs.harvard.edu/abs/2016A&A...596A..97D 596, A97

    De Cia A., Ledoux C., Mattsson L., Petitjean P., Srianand R., Gavignaud I., Jenkins E. B., 2016, @doi [ ] 10.1051/0004-6361/201527895 , https://ui.adsabs.harvard.edu/abs/2016A&A...596A..97D 596, A97

    2016 doi

  44. [52]

    K., 2023, @doi [ ] 10.1093/mnras/stac3702 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.519.4632D 519, 4632

    Di Cesare C., Graziani L., Schneider R., Ginolfi M., Venditti A., Santini P., Hunt L. K., 2023, @doi [ ] 10.1093/mnras/stac3702 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.519.4632D 519, 4632

    2023 doi

  45. [53]

    T., et al., 2023, @doi [ ] 10.1093/mnras/stac3472 , 518, 6011

    Donnan C. T., et al., 2023, @doi [ ] 10.1093/mnras/stac3472 , 518, 6011

    2023 doi

  46. [54]

    T., et al., 2024, @doi [ ] 10.1093/mnras/stae2037 , 533, 3222

    Donnan C. T., et al., 2024, @doi [ ] 10.1093/mnras/stae2037 , 533, 3222

    2024 doi

  47. [55]

    T., 2003, @doi [ ] 10.1146/annurev.astro.41.011802.094840 , 41, 241

    Draine B. T., 2003, @doi [ ] 10.1146/annurev.astro.41.011802.094840 , 41, 241

    2003 doi arXiv

  48. [56]

    T., Lee H

    Draine B. T., Lee H. M., 1984, @doi [ ] 10.1086/162480 , https://ui.adsabs.harvard.edu/abs/1984ApJ...285...89D 285, 89

    1984 doi

  49. [57]

    Dubois Y., et al., 2021, @doi [ ] 10.1051/0004-6361/202039429 , https://ui.adsabs.harvard.edu/abs/2021A&A...651A.109D 651, A109

    2021 doi

  50. [58]

    Dubois Y., et al., 2024, @doi [ ] 10.1051/0004-6361/202449784 , https://ui.adsabs.harvard.edu/abs/2024A&A...687A.240D 687, A240

    2024 doi

  51. [59]

    A., Edmunds M

    Dunne L., Eales S. A., Edmunds M. G., 2003, @doi [ ] 10.1046/j.1365-8711.2003.06440.x , https://ui.adsabs.harvard.edu/abs/2003MNRAS.341..589D 341, 589

    2003 doi

  52. [60]

    Dunne L., et al., 2011, @doi [ ] 10.1111/j.1365-2966.2011.19363.x , https://ui.adsabs.harvard.edu/abs/2011MNRAS.417.1510D 417, 1510

    2011 doi

  53. [61]

    J., Gnedin N

    Esmerian C. J., Gnedin N. Y., 2022, @doi [ ] 10.3847/1538-4357/ac9612 , https://ui.adsabs.harvard.edu/abs/2022ApJ...940...74E 940, 74

    2022 doi

  54. [62]

    J., Gnedin N

    Esmerian C. J., Gnedin N. Y., 2024, @doi [ ] 10.3847/1538-4357/ad410f , https://ui.adsabs.harvard.edu/abs/2024ApJ...968..113E 968, 113

    2024 doi

  55. [63]

    L., Fudamoto Y., Oesch P

    Faisst A. L., Fudamoto Y., Oesch P. A., Scoville N., Riechers D. A., Pavesi R., Capak P., 2020, @doi [ ] 10.1093/mnras/staa2545 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.498.4192F 498, 4192

    2020 doi

  56. [64]

    Feldmann R., et al., 2023, @doi [ ] 10.1093/mnras/stad1205 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.522.3831F 522, 3831

    2023 doi

  57. [65]

    Feldmann R., et al., 2025, @doi [ ] 10.1093/mnras/stae2633 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.536..988F 536, 988

    2025 doi

  58. [66]

    Ferrara A., 2024, @doi [ ] 10.1051/0004-6361/202348321 , https://ui.adsabs.harvard.edu/abs/2024A&A...684A.207F 684, A207

    2024 doi

  59. [67]

    Ferrara A., Pallottini A., Dayal P., 2023, @doi [ ] 10.1093/mnras/stad1095 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.522.3986F 522, 3986

    2023 doi

  60. [68]

    Ferrara A., Pallottini A., Sommovigo L., 2025, @doi [ ] 10.1051/0004-6361/202452707 , https://ui.adsabs.harvard.edu/abs/2025A&A...694A.286F 694, A286

    2025 doi

  61. [69]

    L., et al., 2022, @doi [ ] 10.3847/2041-8213/ac966e , https://ui.adsabs.harvard.edu/abs/2022ApJ...940L..55F 940, L55

    Finkelstein S. L., et al., 2022, @doi [ ] 10.3847/2041-8213/ac966e , https://ui.adsabs.harvard.edu/abs/2022ApJ...940L..55F 940, L55

    2022 doi

  62. [70]

    Fiore F., Ferrara A., Bischetti M., Feruglio C., Travascio A., 2023, @doi [ ] 10.3847/2041-8213/acb5f2 , https://ui.adsabs.harvard.edu/abs/2023ApJ...943L..27F 943, L27

    2023 doi

  63. [71]

    Fisher R., et al., 2025, @doi [ ] 10.1093/mnras/staf485 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.539..109F 539, 109

    2025 doi

  64. [72]

    Fudamoto Y., et al., 2020, @doi [ ] 10.1051/0004-6361/202038163 , https://ui.adsabs.harvard.edu/abs/2020A&A...643A...4F 643, A4

    2020 doi

  65. [73]

    Fujimoto S., et al., 2023, @doi [ ] 10.3847/2041-8213/acd2d9 , https://ui.adsabs.harvard.edu/abs/2023ApJ...949L..25F 949, L25

    2023 doi

  66. [74]

    Fujimoto S., et al., 2024, @doi [ ] 10.3847/1538-4357/ad9027 , https://ui.adsabs.harvard.edu/abs/2024ApJ...977..250F 977, 250

    2024 doi

  67. [75]

    Garaldi E., Kannan R., Smith A., Springel V., Pakmor R., Vogelsberger M., Hernquist L., 2022, @doi [ ] 10.1093/mnras/stac257 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.512.4909G 512, 4909

    2022 doi

  68. [76]

    Garaldi E., et al., 2024, @doi [ ] 10.1093/mnras/stae839 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.530.3765G 530, 3765

    2024 doi

  69. [77]

    Y., 2014, @doi [ ] 10.1088/0004-637X/793/1/29 , http://adsabs.harvard.edu/abs/2014ApJ...793...29G 793, 29

    Gnedin N. Y., 2014, @doi [ ] 10.1088/0004-637X/793/1/29 , http://adsabs.harvard.edu/abs/2014ApJ...793...29G 793, 29

    2014 doi

  70. [78]

    D., Meurer G., Heckman T

    Goldader J. D., Meurer G., Heckman T. M., Seibert M., Sanders D. B., Calzetti D., Steidel C. C., 2002, @doi [ ] 10.1086/339165 , https://ui.adsabs.harvard.edu/abs/2002ApJ...568..651G 568, 651

    2002 doi

  71. [79]

    L., et al., 2021, @doi [ ] 10.1093/mnras/stab362 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.503..511G 503, 511

    Granato G. L., et al., 2021, @doi [ ] 10.1093/mnras/stab362 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.503..511G 503, 511

    2021 doi

  72. [80]

    K., Maio U., Glatzle M., Ciardi B., 2020, @doi [ ] 10.1093/mnras/staa796 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.494.1071G 494, 1071

    Graziani L., Schneider R., Ginolfi M., Hunt L. K., Maio U., Glatzle M., Ciardi B., 2020, @doi [ ] 10.1093/mnras/staa796 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.494.1071G 494, 1071

    2020 doi

  73. [81]

    Groenewegen M. A. T., 1997, , https://ui.adsabs.harvard.edu/abs/1997A&A...317..503G 317, 503

    1997

  74. [82]

    Harikane Y., et al., 2020, @doi [ ] 10.3847/1538-4357/ab94bd , https://ui.adsabs.harvard.edu/abs/2020ApJ...896...93H 896, 93

    2020 doi

  75. [83]

    Harikane Y., et al., 2023a, @doi [ ] 10.3847/1538-4365/acaaa9 , https://ui.adsabs.harvard.edu/abs/2023ApJS..265....5H 265, 5

    doi

  76. [84]

    Harikane Y., Nakajima K., Ouchi M., Umeda H., Isobe Y., Ono Y., Xu Y., Zhang Y., 2023b, @doi [ ] 10.3847/1538-4357/ad0b7e , 960, 56

    doi

  77. [85]

    Hashimoto T., et al., 2019, @doi [ ] 10.1093/pasj/psz049 , https://ui.adsabs.harvard.edu/abs/2019PASJ...71...71H 71, 71

    2019 doi

  78. [86]

    Herrera-Camus R., et al., 2025, @doi [ ] 10.1051/0004-6361/202553896 , https://ui.adsabs.harvard.edu/abs/2025A&A...699A..80H 699, A80

    2025 doi

  79. [87]

    Hirashita H., 2000, @doi [ ] 10.1093/pasj/52.4.585 , https://ui.adsabs.harvard.edu/abs/2000PASJ...52..585H 52, 585

    2000 doi

  80. [88]

    Hirashita H., Aoyama S., 2019, @doi [ ] 10.1093/mnras/sty2838 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.482.2555H 482, 2555

    2019 doi

  81. [89]

    F., 1979, @doi [ ] 10.1086/190631 , https://ui.adsabs.harvard.edu/abs/1979ApJS...41..555H 41, 555

    Hollenbach D., McKee C. F., 1979, @doi [ ] 10.1086/190631 , https://ui.adsabs.harvard.edu/abs/1979ApJS...41..555H 41, 555

    1979 doi

  82. [90]

    Y.-Y., et al., 2024, @doi [ ] 10.3847/1538-4357/ad5da8 , https://ui.adsabs.harvard.edu/abs/2024ApJ...973....8H 973, 8

    Hsiao T. Y.-Y., et al., 2024, @doi [ ] 10.3847/1538-4357/ad5da8 , https://ui.adsabs.harvard.edu/abs/2024ApJ...973....8H 973, 8

    2024 doi

  83. [91]

    S., Naab T., 2019, @doi [ ] 10.1093/mnras/stz1481 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.487.3252H 487, 3252

    Hu C.-Y., Zhukovska S., Somerville R. S., Naab T., 2019, @doi [ ] 10.1093/mnras/stz1481 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.487.3252H 487, 3252

    2019 doi

  84. [92]

    D., 2007, Computing In Science & Engineering, 9, 90

    Hunter J. D., 2007, Computing In Science & Engineering, 9, 90

    2007

  85. [93]

    D., Conroy C., Behroozi P., 2018, @doi [ ] 10.3847/1538-4357/aaa3f0 , https://ui.adsabs.harvard.edu/abs/2018ApJ...854...36I 854, 36

    Imara N., Loeb A., Johnson B. D., Conroy C., Behroozi P., 2018, @doi [ ] 10.3847/1538-4357/aaa3f0 , https://ui.adsabs.harvard.edu/abs/2018ApJ...854...36I 854, 36

    2018 doi

  86. [94]

    Inami H., et al., 2022, @doi [ ] 10.1093/mnras/stac1779 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.515.3126I 515, 3126

    2022 doi

  87. [95]

    I., Schaerer D., Thuan T

    Izotov Y. I., Schaerer D., Thuan T. X., Worseck G., Guseva N., 2016a, @doi [ ] 10.1093/mnras/stw1205 , 461, 3683

    doi

  88. [96]

    I., Orlitova I., Schaerer D., Thuan T

    Izotov Y. I., Orlitova I., Schaerer D., Thuan T. X., Verhamme A., Guseva N., Worseck G., 2016b, @doi [Nature] 10.1038/nature16456 , 529, 178

    doi

  89. [97]

    B., 2009, @doi [ ] 10.1088/0004-637X/700/2/1299 , https://ui.adsabs.harvard.edu/abs/2009ApJ...700.1299J 700, 1299

    Jenkins E. B., 2009, @doi [ ] 10.1088/0004-637X/700/2/1299 , https://ui.adsabs.harvard.edu/abs/2009ApJ...700.1299J 700, 1299

    2009 doi

  90. [98]

    Jolly J.-B., et al., 2025, @doi [ ] 10.1051/0004-6361/202346239 , https://ui.adsabs.harvard.edu/abs/2025A&A...693A.190J 693, A190

    2025 doi

  91. [99]

    Jones E., Oliphant T., Peterson P., et al., 2001, SciPy : Open source scientific tools for Python , http://www.scipy.org/

    2001

  92. [100]

    Jones E., Smith B., Dav \'e R., Narayanan D., Li Q., 2024, @doi [ ] 10.1093/mnras/stae2445 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.535.1293J 535, 1293

    2024 doi

  93. [101]

    Kannan R., Vogelsberger M., Marinacci F., McKinnon R., Pakmor R., Springel V., 2019, @doi [ ] 10.1093/mnras/stz287 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.485..117K 485, 117

    2019 doi

  94. [102]

    Kannan R., Garaldi E., Smith A., Pakmor R., Springel V., Vogelsberger M., Hernquist L., 2022, @doi [ ] 10.1093/mnras/stab3710 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.511.4005K 511, 4005

    2022 doi

  95. [103]

    Kannan R., et al., 2025, @doi [The Open Journal of Astrophysics] 10.33232/001c.145804 , https://ui.adsabs.harvard.edu/abs/2025OJAp....8E.153K 8, 153

    2025 doi

  96. [104]

    U., et al., 2023, @doi [ ] 10.1093/mnras/stad2977 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.526.3871K 526, 3871

    Kapoor A. U., et al., 2023, @doi [ ] 10.1093/mnras/stad2977 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.526.3871K 526, 3871

    2023 doi

  97. [105]

    U., et al., 2024, @doi [ ] 10.1051/0004-6361/202451207 , https://ui.adsabs.harvard.edu/abs/2024A&A...692A..79K 692, A79

    Kapoor A. U., et al., 2024, @doi [ ] 10.1051/0004-6361/202451207 , https://ui.adsabs.harvard.edu/abs/2024A&A...692A..79K 692, A79

    2024 doi

  98. [106]

    Katz H., et al., 2023, @doi [ ] 10.1093/mnras/stac3019 , 518, 270

    2023 doi

  99. [107]

    Khusanova Y., et al., 2021, @doi [ ] 10.1051/0004-6361/202038944 , https://ui.adsabs.harvard.edu/abs/2021A&A...649A.152K 649, A152

    2021 doi

  100. [108]

    Killi M., et al., 2024, @doi [ ] 10.1093/mnras/stae1371 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.531.3222K 531, 3222

    2024 doi

  101. [109]

    Kim J., et al., 2021, @doi [ ] 10.1093/mnras/stab878 , 504, 487

    2021 doi

  102. [110]

    Kimm T., Bieri R., Geen S., Rosdahl J., Blaizot J., Michel-Dansac L., Garel T., 2022, @doi [ ] 10.3847/1538-4365/ac426d , https://ui.adsabs.harvard.edu/abs/2022ApJS..259...21K 259, 21

    2022 doi

  103. [111]

    Kostyuk I., Nelson D., Ciardi B., Glatzle M., Pillepich A., 2023, @doi [ ] 10.1093/mnras/stad677 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.521.3077K 521, 3077

    2023 doi

  104. [112]

    arXiv:2405.04578

    Kravtsov A., Belokurov V., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2405.04578 , https://ui.adsabs.harvard.edu/abs/2024arXiv240504578K p. arXiv:2405.04578

    2024 doi arXiv

  105. [113]

    J., Lada E

    Lada C. J., Lada E. A., 2003, @doi [ ] 10.1146/annurev.astro.41.011802.094844 , https://ui.adsabs.harvard.edu/abs/2003ARA&A..41...57L 41, 57

    2003 doi arXiv

  106. [114]

    T., 1993, @doi [ ] 10.1086/172149 , https://ui.adsabs.harvard.edu/abs/1993ApJ...402..441L 402, 441

    Laor A., Draine B. T., 1993, @doi [ ] 10.1086/172149 , https://ui.adsabs.harvard.edu/abs/1993ApJ...402..441L 402, 441

    1993 doi

  107. [115]

    Le F \`e vre O., et al., 2020, @doi [ ] 10.1051/0004-6361/201936965 , https://ui.adsabs.harvard.edu/abs/2020A&A...643A...1L 643, A1

    2020 doi

  108. [116]

    N., Thaddeus P., 1989, @doi [ ] 10.1086/191357 , https://ui.adsabs.harvard.edu/abs/1989ApJS...70..731L 70, 731

    Leisawitz D., Bash F. N., Thaddeus P., 1989, @doi [ ] 10.1086/191357 , https://ui.adsabs.harvard.edu/abs/1989ApJS...70..731L 70, 731

    1989 doi

  109. [117]

    Leung G. C. K., et al., 2023, @doi [ ] 10.3847/2041-8213/acf365 , 954, L46

    2023 doi

  110. [118]

    Lewis J. S. W., et al., 2022, @doi [ ] 10.1093/mnras/stac2383 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.516.3389L 516, 3389

    2022 doi

  111. [119]

    Lewis J. S. W., Ocvirk P., Dubois Y., Aubert D., Chardin J., Gillet N., Th \'e lie \'E ., 2023, @doi [ ] 10.1093/mnras/stad081 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.519.5987L 519, 5987

    2023 doi

  112. [120]

    Li Q., Narayanan D., Dav \'e R., 2019, @doi [ ] 10.1093/mnras/stz2684 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.490.1425L 490, 1425

    2019 doi

  113. [121]

    Li Q., Narayanan D., Torrey P., Davé R., Vogelsberger M., 2021, @doi [ ] 10.1093/mnras/stab2196 , 507, 548

    2021 doi

  114. [122]

    Liu Z., et al., 2024, @doi [ ] 10.3847/1538-4357/ad4096 , https://ui.adsabs.harvard.edu/abs/2024ApJ...968...15L 968, 15

    2024 doi

  115. [123]

    J., et al., 2024, @doi [Nature] 10.1038/s41586-024-07227-0 , 627, 48

    Looser T. J., et al., 2024, @doi [Nature] 10.1038/s41586-024-07227-0 , 627, 48

    2024 doi

  116. [124]

    C., Vijayan A

    Lovell C. C., Vijayan A. P., Thomas P. A., Wilkins S. M., Barnes D. J., Irodotou D., Roper W., 2021, @doi [ ] 10.1093/mnras/staa3360 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.500.2127L 500, 2127

    2021 doi

  117. [125]

    Ma X., et al., 2018, @doi [ ] 10.1093/mnras/sty1024 , 478, 1694

    2018 doi

  118. [126]

    arXiv:2504.15346

    Maheson G., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2504.15346 , https://ui.adsabs.harvard.edu/abs/2025arXiv250415346M p. arXiv:2504.15346

    2025 doi arXiv

  119. [127]

    K., 2015, @doi [ ] 10.1093/mnrasl/slv070 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.451L..70M 451, L70

    Mancini M., Schneider R., Graziani L., Valiante R., Dayal P., Maio U., Ciardi B., Hunt L. K., 2015, @doi [ ] 10.1093/mnrasl/slv070 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.451L..70M 451, L70

    2015 doi

  120. [128]

    Marinacci F., et al., 2018, @doi [ ] 10.1093/mnras/sty2206 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.480.5113M 480, 5113

    2018 doi

  121. [129]

    V., Vogelsberger M., Torrey P., Springel V., 2019, @doi [ ] 10.1093/mnras/stz2391 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.489.4233M 489, 4233

    Marinacci F., Sales L. V., Vogelsberger M., Torrey P., Springel V., 2019, @doi [ ] 10.1093/mnras/stz2391 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.489.4233M 489, 4233

    2019 doi

  122. [130]

    D., Sommovigo L., Kohandel M., 2025a, @doi [Nature Astronomy] 10.1038/s41550-024-02426-1 , https://ui.adsabs.harvard.edu/abs/2025NatAs...9..458M 9, 458

    Markov V., Gallerani S., Ferrara A., Pallottini A., Parlanti E., Mascia F. D., Sommovigo L., Kohandel M., 2025a, @doi [Nature Astronomy] 10.1038/s41550-024-02426-1 , https://ui.adsabs.harvard.edu/abs/2025NatAs...9..458M 9, 458

    doi

  123. [131]

    Markov V., et al., 2025b, @doi [ ] 10.1051/0004-6361/202555182 , https://ui.adsabs.harvard.edu/abs/2025A&A...702A..33M 702, A33

    doi

  124. [132]

    Mart \' nez-Gonz \'a lez S., Silich S., Tenorio-Tagle G., 2021, @doi [ ] 10.1093/mnras/stab2190 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.507.1175M 507, 1175

    2021 doi

  125. [133]

    McClymont W., et al., 2025a, @doi [ ] 10.1093/mnras/staf1660 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.544..513M 544, 513

    doi

  126. [134]

    McClymont W., et al., 2025b, @doi [ ] 10.1093/mnras/staf1861 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.544.1732M 544, 1732

    doi

  127. [135]

    McClymont W., et al., 2026, @doi [ ] 10.1093/mnras/stag016 , https://ui.adsabs.harvard.edu/abs/2026MNRAS.tmp...20M

    2026 doi

  128. [136]

    McKinnon R., Torrey P., Vogelsberger M., 2016, @doi [ ] 10.1093/mnras/stw253 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.457.3775M 457, 3775

    2016 doi

  129. [137]

    C., Marinacci F., 2017, @doi [ ] 10.1093/mnras/stx467 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.468.1505M 468, 1505

    McKinnon R., Torrey P., Vogelsberger M., Hayward C. C., Marinacci F., 2017, @doi [ ] 10.1093/mnras/stx467 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.468.1505M 468, 1505

    2017 doi

  130. [138]

    McKinnon R., Vogelsberger M., Torrey P., Marinacci F., Kannan R., 2018, @doi [ ] 10.1093/mnras/sty1248 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.478.2851M 478, 2851

    2018 doi

  131. [139]

    J., et al., 2024, @doi [ ] 10.1093/mnras/stad3471 , 527, 5004

    McLeod D. J., et al., 2024, @doi [ ] 10.1093/mnras/stad3471 , 527, 5004

    2024 doi

  132. [140]

    Mitsuhashi I., et al., 2024, @doi [ ] 10.3847/1538-4357/ad5675 , https://ui.adsabs.harvard.edu/abs/2024ApJ...971..161M 971, 161

    2024 doi

  133. [141]

    C., Leja J., Foreman-Mackey D., Hayward C

    Nagaraj G., Forbes J. C., Leja J., Foreman-Mackey D., Hayward C. C., 2022, @doi [ ] 10.3847/1538-4357/ac9477 , https://ui.adsabs.harvard.edu/abs/2022ApJ...939...29N 939, 29

    2022 doi

  134. [142]

    P., et al., 2022, @doi [ ] 10.3847/2041-8213/ac9b22 , https://ui.adsabs.harvard.edu/abs/2022ApJ...940L..14N 940, L14

    Naidu R. P., et al., 2022, @doi [ ] 10.3847/2041-8213/ac9b22 , https://ui.adsabs.harvard.edu/abs/2022ApJ...940L..14N 940, L14

    2022 doi

  135. [143]

    P., et al., 2018, @doi [ ] 10.1093/mnras/sty618 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.477.1206N 477, 1206

    Naiman J. P., et al., 2018, @doi [ ] 10.1093/mnras/sty618 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.477.1206N 477, 1206

    2018 doi

  136. [144]

    Narayanan D., et al., 2023, @doi [ ] 10.3847/1538-4357/accf8d , https://ui.adsabs.harvard.edu/abs/2023ApJ...951..100N 951, 100

    2023 doi

  137. [145]

    Narayanan D., et al., 2025, @doi [ ] 10.3847/1538-4357/adb41c , https://ui.adsabs.harvard.edu/abs/2025ApJ...982....7N 982, 7

    2025 doi

  138. [146]

    Narayanan D., et al., 2026, @doi [The Open Journal of Astrophysics] 10.33232/001c.159986 , https://ui.adsabs.harvard.edu/abs/2026OJAp....959986N 9, 59986

    2026 doi

  139. [147]

    F., Frenk C

    Navarro J. F., Frenk C. S., White S. D. M., 1997, @doi [ ] 10.1086/304888 , 490, 493

    1997 doi

  140. [148]

    Nelson D., et al., 2018, @doi [ ] 10.1093/mnras/stx3040 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.475..624N 475, 624

    2018 doi

  141. [149]

    Novak M., et al., 2017, @doi [ ] 10.1051/0004-6361/201629436 , https://ui.adsabs.harvard.edu/abs/2017A&A...602A...5N 602, A5

    2017 doi

  142. [150]

    Nozawa T., Kozasa T., Habe A., Dwek E., Umeda H., Tominaga N., Maeda K., Nomoto K., 2007, @doi [ ] 10.1086/520621 , https://ui.adsabs.harvard.edu/abs/2007ApJ...666..955N 666, 955

    2007 doi

  143. [151]

    Ocvirk P., et al., 2025, @doi [ ] 10.1051/0004-6361/202452098 , https://ui.adsabs.harvard.edu/abs/2025A&A...703A..98O 703, A98

    2025 doi

  144. [152]

    Oku Y., Nagamine K., 2024, @doi [ ] 10.3847/1538-4357/ad77d3 , https://ui.adsabs.harvard.edu/abs/2024ApJ...975..183O 975, 183

    2024 doi

  145. [153]

    J., Shapley A., Steidel C

    Pahl A. J., Shapley A., Steidel C. C., Reddy N. A., Chen Y., Rudie G. C., Strom A. L., 2023, @doi [ ] 10.1093/mnras/stad774 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.521.3247P 521, 3247

    2023 doi

  146. [154]

    Pallottini A., et al., 2022, @doi [ ] 10.1093/mnras/stac1281 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.513.5621P 513, 5621

    2022 doi

  147. [155]

    arXiv:2504.10585

    Parente M., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2504.10585 , https://ui.adsabs.harvard.edu/abs/2025arXiv250410585P p. arXiv:2504.10585

    2025 doi arXiv

  148. [156]

    C., 2020, @doi [ ] 10.1146/annurev-astro-021820-120014 , https://ui.adsabs.harvard.edu/abs/2020ARA&A..58..363P 58, 363

    P \'e roux C., Howk J. C., 2020, @doi [ ] 10.1146/annurev-astro-021820-120014 , https://ui.adsabs.harvard.edu/abs/2020ARA&A..58..363P 58, 363

    2020 doi

  149. [157]

    C., 2023, @doi [ ] 10.1093/mnras/stad1235 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.522.4852P 522, 4852

    P \'e roux C., De Cia A., Howk J. C., 2023, @doi [ ] 10.1093/mnras/stad1235 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.522.4852P 522, 4852

    2023 doi

  150. [158]

    Pillepich A., et al., 2018, @doi [ ] 10.1093/mnras/stx3112 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.475..648P 475, 648

    2018 doi

  151. [159]

    Popping G., P \'e roux C., 2022, @doi [ ] 10.1093/mnras/stac695 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.513.1531P 513, 1531

    2022 doi

  152. [160]

    S., Galametz M., 2017, @doi [ ] 10.1093/mnras/stx1545 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.471.3152P 471, 3152

    Popping G., Somerville R. S., Galametz M., 2017, @doi [ ] 10.1093/mnras/stx1545 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.471.3152P 471, 3152

    2017 doi

  153. [161]

    F., McMillan S

    Portegies Zwart S. F., McMillan S. L. W., Gieles M., 2010, @doi [ ] 10.1146/annurev-astro-081309-130834 , https://ui.adsabs.harvard.edu/abs/2010ARA&A..48..431P 48, 431

    2010 doi

  154. [162]

    Pozzi F., Calura F., Zamorani G., Delvecchio I., Gruppioni C., Santini P., 2020, @doi [ ] 10.1093/mnras/stz2724 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.491.5073P 491, 5073

    2020 doi

  155. [163]

    D., Chawner H., Barlow M

    Priestley F. D., Chawner H., Barlow M. J., De Looze I., Gomez H. L., Matsuura M., 2022, @doi [ ] 10.1093/mnras/stac2408 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.516.2314P 516, 2314

    2022 doi

  156. [164]

    Pruto G., et al., 2026, @doi [ ] 10.1093/mnras/stag064 , https://ui.adsabs.harvard.edu/abs/2026MNRAS.546ag064P 546, stag064

    2026 doi

  157. [165]

    G., et al., 2023, @doi [ ] 10.3847/2041-8213/acd9d0 , 951, L1

    Pérez-González P. G., et al., 2023, @doi [ ] 10.3847/2041-8213/acd9d0 , 951, L1

    2023 doi

  158. [166]

    A., et al., 2026, @doi [ ] 10.3847/1538-4357/ae38da , https://ui.adsabs.harvard.edu/abs/2026ApJ...999...15R 999, 15

    Reddy N. A., et al., 2026, @doi [ ] 10.3847/1538-4357/ae38da , https://ui.adsabs.harvard.edu/abs/2026ApJ...999...15R 999, 15

    2026 doi

  159. [167]

    Rela \ n o M., et al., 2022, @doi [ ] 10.1093/mnras/stac2108 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.515.5306R 515, 5306

    2022 doi

  160. [168]

    R \'e my-Ruyer A., et al., 2014, @doi [ ] 10.1051/0004-6361/201322803 , 563, A31

    2014 doi

  161. [169]

    E., et al., 2023, @doi [Nature Astronomy] 10.1038/s41550-023-01921-1 , https://ui.adsabs.harvard.edu/abs/2023NatAs...7..611R 7, 611

    Robertson B. E., et al., 2023, @doi [Nature Astronomy] 10.1038/s41550-023-01921-1 , https://ui.adsabs.harvard.edu/abs/2023NatAs...7..611R 7, 611

    2023 doi

  162. [170]

    Robertson B., et al., 2024, @doi [ ] 10.3847/1538-4357/ad463d , 970, 31

    2024 doi

  163. [171]

    Rosdahl J., et al., 2018, @doi [ ] 10.1093/mnras/sty1655 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.479..994R 479, 994

    2018 doi

  164. [172]

    Rosdahl J., et al., 2022, @doi [ ] 10.1093/mnras/stac1942 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.515.2386R 515, 2386

    2022 doi

  165. [173]

    Rowlands K., et al., 2014, @doi [ ] 10.1093/mnras/stu510 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.441.1017R 441, 1017

    2014 doi

  166. [174]

    C., 2018, @doi [ ] 10.3847/1538-4357/aabf3c , https://ui.adsabs.harvard.edu/abs/2018ApJ...859...11S 859, 11

    Salim S., Boquien M., Lee J. C., 2018, @doi [ ] 10.3847/1538-4357/aabf3c , https://ui.adsabs.harvard.edu/abs/2018ApJ...859...11S 859, 11

    2018 doi

  167. [175]

    Schaerer D., et al., 2015, @doi [ ] 10.1051/0004-6361/201424649 , 574, A19

    2015 doi

  168. [176]

    Schaye J., et al., 2026, @doi [ ] 10.1093/mnras/stag375 , https://ui.adsabs.harvard.edu/abs/2026MNRAS.548ag375S 548, stag375

    2026 doi

  169. [177]

    K., 2024, @doi [ ] 10.1146/annurev-astro-071221-052651 , https://ui.adsabs.harvard.edu/abs/2024ARA&A..62..369S 62, 369

    Schinnerer E., Leroy A. K., 2024, @doi [ ] 10.1146/annurev-astro-071221-052651 , https://ui.adsabs.harvard.edu/abs/2024ARA&A..62..369S 62, 369

    2024 doi

  170. [178]

    Schouws S., et al., 2025, @doi [ ] 10.3847/1538-4357/adbf1b , https://ui.adsabs.harvard.edu/abs/2025ApJ...988...19S 988, 19

    2025 doi

  171. [179]

    Schreiber C., Elbaz D., Pannella M., Ciesla L., Wang T., Franco M., 2018, @doi [ ] 10.1051/0004-6361/201731506 , https://ui.adsabs.harvard.edu/abs/2018A&A...609A..30S 609, A30

    2018 doi

  172. [180]

    A., 2025, @doi [ ] 10.3847/1538-4365/ae0cc6 , https://ui.adsabs.harvard.edu/abs/2025ApJS..281...37S 281, 37

    Semenov V. A., 2025, @doi [ ] 10.3847/1538-4365/ae0cc6 , https://ui.adsabs.harvard.edu/abs/2025ApJS..281...37S 281, 37

    2025 doi

  173. [181]

    A., Conroy C., Hernquist L., 2025, @doi [ ] 10.3847/1538-4357/ade22d , https://ui.adsabs.harvard.edu/abs/2025ApJ...989..219S 989, 219

    Semenov V. A., Conroy C., Hernquist L., 2025, @doi [ ] 10.3847/1538-4357/ade22d , https://ui.adsabs.harvard.edu/abs/2025ApJ...989..219S 989, 219

    2025 doi

  174. [182]

    Shen X., Vogelsberger M., Nelson D., Tacchella S., Hernquist L., Springel V., Marinacci F., Torrey P., 2022, @doi [ ] 10.1093/mnras/stab3794 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.510.5560S 510, 5560

    2022 doi

  175. [183]

    Shen X., Vogelsberger M., Boylan-Kolchin M., Tacchella S., Kannan R., 2023, @doi [ ] 10.1093/mnras/stad2508 , 525, 3254

    2023 doi

  176. [184]

    Shen X., et al., 2026, @doi [ ] 10.1093/mnras/staf2119 , https://ui.adsabs.harvard.edu/abs/2026MNRAS.545f2119S 545, staf2119

    2026 doi

  177. [185]

    D., Dwek E., Mac Low M.-M., Hill A

    Slavin J. D., Dwek E., Mac Low M.-M., Hill A. S., 2020, @doi [ ] 10.3847/1538-4357/abb5a4 , https://ui.adsabs.harvard.edu/abs/2020ApJ...902..135S 902, 135

    2020 doi

  178. [186]

    L., Hopkins P

    Smith A., Ma X., Bromm V., Finkelstein S. L., Hopkins P. F., Faucher-Gigu \`e re C.-A., Kere s D., 2019, @doi [ ] 10.1093/mnras/sty3483 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.484...39S 484, 39

    2019 doi

  179. [187]

    Smith A., Kannan R., Garaldi E., Vogelsberger M., Pakmor R., Springel V., Hernquist L., 2022, @doi [ ] 10.1093/mnras/stac713 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.512.3243S 512, 3243

    2022 doi

  180. [188]

    Sommovigo L., Algera H., 2025, @doi [ ] 10.1093/mnras/staf897 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.540.3693S 540, 3693

    2025 doi

  181. [189]

    Sommovigo L., et al., 2022a, @doi [ ] 10.1093/mnras/stac302 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.513.3122S 513, 3122

    doi

  182. [190]

    Sommovigo L., et al., 2022b, @doi [ ] 10.1093/mnras/stac2997 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.517.5930S 517, 5930

    doi

  183. [191]

    S., et al., 2023, @doi [ ] 10.1038/s41586-023-05998-6 , https://ui.adsabs.harvard.edu/abs/2023Natur.618..708S 618, 708

    Spilker J. S., et al., 2023, @doi [ ] 10.1038/s41586-023-05998-6 , https://ui.adsabs.harvard.edu/abs/2023Natur.618..708S 618, 708

    2023 doi

  184. [192]

    Springel V., 2010, @doi [ ] 10.1111/j.1365-2966.2009.15715.x , https://ui.adsabs.harvard.edu/abs/2010MNRAS.401..791S 401, 791

    2010 doi

  185. [193]

    Springel V., et al., 2018, @doi [ ] 10.1093/mnras/stx3304 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.475..676S 475, 676

    2018 doi

  186. [194]

    R., Eldridge J

    Stanway E. R., Eldridge J. J., 2018, @doi [ ] 10.1093/mnras/sty1353 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.479...75S 479, 75

    2018 doi

  187. [195]

    Sugahara Y., et al., 2021, @doi [ ] 10.3847/1538-4357/ac2a36 , 923, 5

    2021 doi

  188. [196]

    C., Shen X., Wetzel A., Cochrane R

    Sun G., Faucher-Gigu \`e re C.-A., Hayward C. C., Shen X., Wetzel A., Cochrane R. K., 2023, @doi [ ] 10.3847/2041-8213/acf85a , 955, L35

    2023 doi

  189. [197]

    Tacchella S., et al., 2022, @doi [ ] 10.3847/1538-4357/ac4cad , https://ui.adsabs.harvard.edu/abs/2022ApJ...927..170T 927, 170

    2022 doi

  190. [198]

    Tacchella S., et al., 2023, @doi [ ] 10.3847/1538-4357/acdbc6 , https://ui.adsabs.harvard.edu/abs/2023ApJ...952...74T 952, 74

    2023 doi

  191. [199]

    Tamura Y., et al., 2019, @doi [ ] 10.3847/1538-4357/ab0374 , https://ui.adsabs.harvard.edu/abs/2019ApJ...874...27T 874, 27

    2019 doi

  192. [200]

    W., et al., 2026, @doi [ ] 10.1093/mnras/staf2040 , https://ui.adsabs.harvard.edu/abs/2026MNRAS.545f2040T 545, staf2040

    Trayford J. W., et al., 2026, @doi [ ] 10.1093/mnras/staf2040 , https://ui.adsabs.harvard.edu/abs/2026MNRAS.545f2040T 545, staf2040

    2026 doi

  193. [201]

    Trebitsch M., et al., 2021, @doi [ ] 10.1051/0004-6361/202037698 , https://ui.adsabs.harvard.edu/abs/2021A&A...653A.154T 653, A154

    2021 doi

  194. [202]

    P., Sun G., Chung D

    Viero M. P., Sun G., Chung D. T., Moncelsi L., Condon S. S., 2022, @doi [ ] 10.1093/mnrasl/slac075 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.516L..30V 516, L30

    2022 doi

  195. [203]

    P., Clay S

    Vijayan A. P., Clay S. J., Thomas P. A., Yates R. M., Wilkins S. M., Henriques B. M., 2019, @doi [ ] 10.1093/mnras/stz1948 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.489.4072V 489, 4072

    2019 doi

  196. [204]

    Villanueva V., et al., 2024, @doi [ ] 10.1051/0004-6361/202451490 , https://ui.adsabs.harvard.edu/abs/2024A&A...691A.133V 691, A133

    2024 doi

  197. [205]

    Vlahakis C., Dunne L., Eales S., 2005, @doi [ ] 10.1111/j.1365-2966.2005.09666.x , https://ui.adsabs.harvard.edu/abs/2005MNRAS.364.1253V 364, 1253

    2005 doi

  198. [206]

    M., et al., 2026, @doi [ ] 10.3847/1538-4357/ae38b7 , https://ui.adsabs.harvard.edu/abs/2026ApJ...998..215W 998, 215

    Wainer T. M., et al., 2026, @doi [ ] 10.3847/1538-4357/ae38b7 , https://ui.adsabs.harvard.edu/abs/2026ApJ...998..215W 998, 215

    2026 doi

  199. [207]

    Walt S. v. d., Colbert S. C., Varoquaux G., 2011, Computing in Science & Engineering, 13, 22

    2011

  200. [208]

    Wang B., et al., 2023, @doi [ ] 10.3847/2041-8213/acfe07 , 957, L34

    2023 doi

  201. [209]

    Wang Z., et al., 2025, @doi [ ] 10.1093/mnras/staf1677 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.544.2675W 544, 2675

    2025 doi

  202. [210]

    K., Richard J., Gallazzi A., Micha owski M

    Watson D., Christensen L., Knudsen K. K., Richard J., Gallazzi A., Micha owski M. J., 2015, @doi [ ] 10.1038/nature14164 , https://ui.adsabs.harvard.edu/abs/2015Natur.519..327W 519, 327

    2015 doi

  203. [211]

    Weinberger R., Springel V., Pakmor R., 2020, @doi [ ] 10.3847/1538-4365/ab908c , https://ui.adsabs.harvard.edu/abs/2020ApJS..248...32W 248, 32

    2020 doi

  204. [212]

    Whitler L., et al., 2025, @doi [ ] 10.3847/1538-4357/adfddc , https://ui.adsabs.harvard.edu/abs/2025ApJ...992...63W 992, 63

    2025 doi

  205. [213]

    C., Zhang Q., 2002, @doi [The Astronomical Journal] 10.1086/341822 , 124, 1418

    Whitmore B. C., Zhang Q., 2002, @doi [The Astronomical Journal] 10.1086/341822 , 124, 1418

    2002 doi

  206. [214]

    M., Fleischer A

    Winters J. M., Fleischer A. J., Le Bertre T., Sedlmayr E., 1997, , https://ui.adsabs.harvard.edu/abs/1997A&A...326..305W 326, 305

    1997

  207. [215]

    M., Greiner J., Fynbo J

    Wiseman P., Schady P., Bolmer J., Kr \"u hler T., Yates R. M., Greiner J., Fynbo J. P. U., 2017, @doi [ ] 10.1051/0004-6361/201629228 , https://ui.adsabs.harvard.edu/abs/2017A&A...599A..24W 599, A24

    2017 doi

  208. [216]

    C., Maiolino R., Smit R., Schneider R., 2023a, @doi [ ] 10.1093/mnras/stad1470 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.523.3119W 523, 3119

    Witstok J., Jones G. C., Maiolino R., Smit R., Schneider R., 2023a, @doi [ ] 10.1093/mnras/stad1470 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.523.3119W 523, 3119

    doi

  209. [217]

    Witstok J., et al., 2023b, @doi [ ] 10.1038/s41586-023-06413-w , https://ui.adsabs.harvard.edu/abs/2023Natur.621..267W 621, 267

    doi

  210. [218]

    Yajima H., Umemura M., Mori M., Nakamoto T., 2009, @doi [ ] 10.1111/j.1365-2966.2009.15195.x , https://ui.adsabs.harvard.edu/abs/2009MNRAS.398..715Y 398, 715

    2009 doi

  211. [219]

    Yasuda Y., Kozasa T., 2012, @doi [ ] 10.1088/0004-637X/745/2/159 , https://ui.adsabs.harvard.edu/abs/2012ApJ...745..159Y 745, 159

    2012 doi

  212. [220]

    A., et al., 2021, @doi [ ] 10.3847/1538-4357/abdb27 , https://ui.adsabs.harvard.edu/abs/2021ApJ...909..165Z 909, 165

    Zavala J. A., et al., 2021, @doi [ ] 10.3847/1538-4357/abdb27 , https://ui.adsabs.harvard.edu/abs/2021ApJ...909..165Z 909, 165

    2021 doi

  213. [221]

    Zier O., et al., 2025a, @doi [ ] 10.1093/mnras/staf1052 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.544..391Z 544, 391

    doi

  214. [222]

    Zier O., et al., 2025b, @doi [ ] 10.1093/mnras/staf1053 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.544..410Z 544, 410

    doi

  215. [223]

    G., 2004, @doi [ ] 10.1086/382351 , https://ui.adsabs.harvard.edu/abs/2004ApJS..152..211Z 152, 211

    Zubko V., Dwek E., Arendt R. G., 2004, @doi [ ] 10.1086/382351 , https://ui.adsabs.harvard.edu/abs/2004ApJS..152..211Z 152, 211

    2004 doi

  216. [224]

    da Cunha E., et al., 2015, @doi [ ] 10.1088/0004-637X/806/1/110 , https://ui.adsabs.harvard.edu/abs/2015ApJ...806..110D 806, 110

    2015 doi

  217. [225]

    F., et al., 2024, @doi [ ] 10.1093/mnras/stae2171 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.534.2062V 534, 2062

    van Leeuwen I. F., et al., 2024, @doi [ ] 10.1093/mnras/stae2171 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.534.2062V 534, 2062

    2024 doi

  218. [226]

    van der Velden E., 2020, @doi [The Journal of Open Source Software] 10.21105/joss.02004 , https://ui.adsabs.harvard.edu/abs/2020JOSS....5.2004V 5, 2004

    2020 doi

Pith tools

Reviewed July 13, 2026 · model on record in the stance chip above.