Pith. sign in

REVIEW 2 major objections 7 minor 196 references

Introducing the Phoebos simulation: galaxy properties at the dawn of galaxy formation

T0 review · 2 major / 7 minor · reviewed 2026-08-06 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read A 100 Mpc simulation with weak stellar feedback reproduces JWST-era galaxy counts, sizes, and star formation at z>8.

desk verdict Phoebos is a valuable new simulation resource and the weak-feedback baseline is worth taking seriously, but the size–mass slope claim rests on an unverified mass-independent offset assumption that needs addressing before that result is secure. read the letter →

arxiv 2507.04927 v1 pith:HBKWAFWI submitted 2025-07-07 astro-ph.GA astro-ph.CO

Floor van Donkelaar , Pedro R. Capelo , Lucio Mayer , Darren S. Reed , Thomas R. Quinn This is my paper · ORCID
classification astro-ph.GAastro-ph.CO
keywords Phoebossimulationhigh-redshiftgalaxiesgalaxyformationstellarfeedbacksizesstarefficiencycosmicdawnJWST
open problems Dark Matter
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

The paper introduces Phoebos, a 100 Mpc cosmological hydrodynamical simulation built to test whether weak stellar feedback can explain the abundance and properties of massive galaxies seen by JWST at $z\gtrsim8$. At variance with most large-volume simulations, Phoebos uses non-equilibrium radiative cooling without an effective equation of state, and its stellar feedback is intentionally mild. The central claim is that this setup reproduces the observed stellar mass function, stellar-to-halo mass relation, size–mass slope, and specific star formation rate without any redshift-dependent calibration, supporting a picture of rapid, highly efficient star formation during cosmic dawn. The authors also report tentative signs that at lower redshift Phoebos overproduces cosmic star formation, suggesting feedback must strengthen with time.

What carries the argument

The central object is the Phoebos simulation itself: a [100 cMpc]^3 box with $2904^{3}$ dark-matter and $1944^{3}$ gas particles, with dark-matter and gas particle masses of $1.360\times10^6\,M_\odot$ and $8.473\times10^5\,M_\odot$, run with a smoothed-particle hydrodynamics code using a Wendland C4 kernel, non-equilibrium primordial cooling with self-shielding, tabulated metal-line cooling, no pressure floor, and stochastic star formation at a density threshold of $1.0\,m_p\,\mathrm{cm^{-3}}$ and efficiency 0.1. The feedback recipe is a blastwave supernova model whose energy injection is weak in the dense, rapidly cooling gas of $z\gtrsim8$ galaxies, because the cooling and dynamical times are shorter than the typical timescale between supernova explosions. That short-timescale argument, rather than a tuning to high-redshift data, is the load-bearing mechanism that lets Phoebos form galaxies fast enough to match JWST observations.

What would settle it

Forward-model the Phoebos galaxies at z~8 into mock JWST images, fit effective radii from the light, and compare the resulting size–mass relation with the observed one without any free shift of the y-intercept; if the slope or normalization still disagrees, the central claim of reproducing the observed size–mass relation is not established.

Watch

Extended reading notes

Core claim

Phoebos is claimed to reproduce, at $z\gtrsim8$ and without any redshift-dependent calibration, the observed stellar mass function, the stellar-to-halo mass relation, the slope of the stellar size–mass relation, and the specific star formation rate distribution. At $z\sim12$ it matches the highest-redshift stellar-to-halo mass constraints better than other current simulations, while at $z\sim8$ its stellar mass function and star formation rates sit within the observational scatter. After accounting for a ~25 per cent offset between half-light and half-mass radii and for resolution-driven size inflation, the slope of the simulated size–mass relation tracks the observed one up to stellar masses around $10^{9.5}\,M_\odot$, in contrast to a strong-feedback comparison simulation. The paper interprets this as evidence that early galaxy growth happens in a weak-feedback regime where gas cools and collapses faster than supernova feedback can respond, making star formation highly efficient.

Load-bearing premise

The comparison assumes that the difference between observed effective radii and simulated half-mass radii is dominated by a mass-independent offset of about 25 per cent plus resolution-driven size inflation, so that after shifting the observed relation's zero-point the slopes can be compared; if the offset varies with mass or is partly physical, the claimed size–mass slope match does not follow.

Editorial extensions

If this is right

  • The abundant massive galaxies JWST finds at $z\gtrsim10$ can be understood within standard structure formation as the product of highly efficient star formation, without requiring modified cosmology or exotic accretion physics.
  • Once galaxy sizes are defined consistently, early galaxies grow in radius with stellar mass along the observed slope, with the overall normalization set by the half-light/half-mass offset and resolution inflation.
  • Galaxies at $z\gtrsim8$ assemble their stellar mass on timescales shorter than the Hubble time, so rapid assembly is the rule rather than the exception during cosmic dawn.
  • The predicted excess of cosmic star formation at lower redshift implies that the weak-feedback regime must be temporary, with feedback becoming stronger at later epochs.
  • Resolving the multi-phase interstellar medium with non-equilibrium cooling appears to be at least as important as the strength of stellar feedback for producing the high-redshift galaxy population.

Reading between the lines

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

  • A direct test of the size claim would be to forward-model Phoebos galaxies into mock JWST images and measure effective radii from the light, rather than assuming a mass-independent 25 per cent offset; if the slope changes when the shift is fitted freely, the match would not survive.
  • The redshift-dependent feedback transition implied by the star-formation excess could be checked by running Phoebos to $z=0$ and comparing its stellar mass function with the local one; a large overprediction would confirm that a stronger low-redshift feedback mode is needed.
  • The weak-feedback, fast-assembly scenario predicts low outflow mass loading and possibly high escape fractions of ionizing radiation from $z\gtrsim8$ galaxies, which future 21-cm reionization observations and JWST/NIRSpec metallicity measurements could test.
  • If feedback effectiveness is as environment- and redshift-dependent as this simulation suggests, simulations calibrated mainly to the local universe may systematically mispredict the earliest galaxies, and the slope of the stellar mass function at $z\gtrsim12$ becomes a sharp discriminator.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 7 minor

Summary. The paper introduces Phoebos, a [100 cMpc]^3 cosmological hydrodynamical simulation with particle masses mDM=1.360e6 Msun and mgas=8.473e5 Msun, designed to study galaxy formation at z~8-12. It uses ChaNGa with multi-phase, non-equilibrium cooling, stochastic star formation with epsilon_SF=0.1, and blastwave supernova feedback, deliberately avoiding an effective equation of state and AGN feedback. The authors compare the simulation with JWST-era observations of the stellar mass function, stellar-to-halo mass relation, cosmic star formation rate density, star-forming main sequence, specific star formation rate, stellar size-mass relation, and HI fractions. They report good agreement for the stellar mass function, SHMR, and sSFR, claim recovery of the observed size-mass slope, and interpret the results as evidence for highly efficient star formation with only weak stellar feedback at z>8. Lower-resolution runs are used for halo-mass-function convergence, and the paper discusses limitations including SFRD overprediction and the need for stronger feedback at lower redshifts.

Significance. If the main claims hold, Phoebos would be a valuable resource: a large-volume simulation that reproduces several independent high-redshift observables without redshift-dependent recalibration, thereby supporting the emerging picture of a weak-feedback, efficient star-formation regime at cosmic dawn. The paper is honest about several discrepancies (e.g., SFRD relative to Bouwens et al. 2023, SHMR relative to Paquereau et al. 2025, the HI fraction drop) and provides convergence checks for halo mass functions. The central interpretive claim, however, partly rests on the size-mass slope comparison, whose validity currently depends on an unverified assumption about a mass-independent offset between simulated half-mass radii and observed effective radii. The no-tuning claim is also complicated by a redshift-dependent cooling floor unique to the Phoebos run. These issues are addressable but must be resolved before the paper's headline conclusions can be fully accepted.

major comments (2)
  1. [§3.1, Fig. 6; also Abstract and §4] The claim that Phoebos 'recovers the observed slope' of the stellar size-mass relation is established by shifting the y-intercept of the Yang et al. (2025) relation (the 'loosely dotted line' in Fig. 6) to align with the simulated half-mass radii. The shift is justified by a mass-independent ~25 per cent half-light-to-half-mass offset plus resolution-driven puffing, but the Phoebos softening is fixed at 0.300 kpc physical for z<9 (Table 1), while the simulated radii in Fig. 6 span roughly 0.1-1 kpc. A fixed softening should inflate the smallest, lowest-mass galaxies proportionally more than the largest ones, making the net offset mass-dependent unless shown otherwise. The GigaEris and MassiveBlackPS points have different softening and resolution and do not constitute a Phoebos resolution sequence for stellar sizes; the PhoebosLR/ULR runs in Appendix A are used only for halo mass functions. Because this is one of the headline successes listed in the abstract, I ask the authors to quantify the mass dependence of the resolution offset (e.g., from a size resolution sequence or from high-resolution zooms of representative Phoebos systems) or to compare mock-observed effective radii before claiming slope recovery.
  2. [§2, footnote 6; §4] Section 4 states that Phoebos succeeds 'without any redshift-dependent calibration or tuning to high-redshift data.' However, Section 2 reports that the Phoebos run uses a cooling temperature floor of 300 K up to z~10, whereas PhoebosLR and PhoebosULR use a floor of 10 K. This is a redshift-dependent modification specific to the main run, and its effect on the z>8 star formation histories, stellar masses, and sizes is not discussed. Please either demonstrate robustness of the headline results to this floor or qualify the no-tuning claim accordingly.
minor comments (7)
  1. [§2, Table 1 and Fig. 2] There is a missing space in 'smoothed-particlehydrodynamics code ChaNGa', and the axis labels use 'M' where 'M☉' would be clearer.
  2. [§3.1, footnote 8] Footnote 8 is grammatically incomplete: 'For a more detailed discussion see e.g. Kravtsov (2013) and Szomoru et al. (2013), the half-light radius...' should be rewritten as one or more complete sentences.
  3. [§3.1] There are typos: 'the radii within Phoebos should be seen considered as an upper limit' and 'Similary, the haloes at z = 12'; please correct both.
  4. [§3.3.1] In the sentence 'especially at = 12, Thesan-Zoom and Phoebos...' the variable z is missing; it should read 'especially at z = 12'.
  5. [§4] The phrase 'treatment of of a relatively weak stellar feedback' contains a duplicated 'of'.
  6. [Figure 1 caption] The caption spells 'MilleniumTNG'; it should be 'MillenniumTNG'.
  7. [§3.4 and Appendix A2] The text says the origin of the HI drop 'will explore potential explanations in subsequent sections,' but the subsequent discussion is brief and confined to Appendix A2; please either expand the discussion or adjust the forward reference.

Circularity Check

0 steps flagged · score 0.0 of 10

No circular derivation: Phoebos outputs are compared to external data with no high-redshift tuning; the y-intercept shift in the size–mass plot is a comparison convention, not a fitted prediction.

full rationale

Phoebos is a forward simulation with subgrid parameters stated as inherited from earlier, lower-redshift work (Romulus25, Stinson et al.) rather than tuned to the z>8 observables it is compared against. The headline comparisons—stellar mass function, stellar-to-halo mass relation, sSFR, and SFRD—are raw simulation outputs confronted with external observational datasets; no quantity entering those comparisons is fitted to the data being reproduced. The only adjustable-looking element is the size–mass comparison in Fig. 6, where the Yang et al. relation is shown with a modified y-intercept to better align with the simulated half-mass radii. This is a post-processing comparison convention, not a model parameter, and the slope being claimed is unaffected by a constant offset, so the slope comparison is not forced by construction. The GigaEris and MassiveBlackPS citations are self-citations, but they are invoked as higher-resolution simulations sharing the same feedback implementation, providing supporting evidence for a resolution-driven offset; the central SMF, SHMR, and sSFR claims do not depend on them. A possible mass dependence of the fixed-softening size inflation is a physical and measurement concern, not a circularity. No step in the paper defines a predicted quantity in terms of the fitted data or reduces a prediction to a fit.

Assumptions & free parameters 5 free parameters · 4 assumptions · 0 invented entities

The ledger shows no invented physical entities. The simulation's novel content is carried by subgrid parameters (epsilon_SF, density threshold, cooling floor, softening, supernova energy coupling) inherited from prior ChaNGa and Romulus work, plus modeling assumptions about cooling tables and neglected feedback. The most fragile entries are the assumptions that neglected feedback channels (photoionization, radiation pressure, AGN) are unimportant at z > 8 and that the size offset is purely resolution and definition driven, both acknowledged by the authors.

free parameters (5)
  • star formation efficiency epsilon_SF = 0.1
    Sets the rate at which cold dense gas is converted to stars (dM*/dt = epsilon_SF Mgas/tdyn) in Section 2. Inherited from earlier Romulus/Stinson calibrations, not tuned to z > 8, but directly controls the stellar mass assembly rate that the paper argues is high.
  • star formation density threshold n_th = 1.0 proton cm^-3 (Phoebos); 0.1 proton cm^-3 (LR and ULR)
    Gas must be colder than 3e4 K and denser than this threshold to form stars. The threshold is resolution-dependent and affects where stars form, hence galaxy sizes and mass functions (Section 2).
  • cooling temperature floor = 300 K up to z ~ 10 in Phoebos; 10 K in LR and ULR
    Footnote 6: the main Phoebos run uses a 300 K floor at early times while lower-resolution runs use 10 K. Suppressing cooling below 300 K can alter gas fragmentation and star formation; a numerical choice with physical consequences.
  • gravitational softening epsilon = 0.300 kpc for z < 9; 3/(1+z) kpc for z >= 9
    Resolution scale (Section 2, Table 1). The paper argues, citing Bate and Burkert (1997), that insufficiently small smoothing relative to softening inflates galaxy sizes, so this parameter directly affects the size comparisons in Figures 6 and 7.
  • Type II supernova thermal energy injection = 1e51 erg per supernova
    Injected as thermal energy with radiative cooling disabled during the blastwave shell survival time (Stinson et al. 2006, Section 2). The effective coupling in high-density gas determines how weak the feedback is, which is the central physical ingredient.
assumptions (4)
  • domain assumption Lambda-CDM cosmology with Planck 2018 parameters (Omega_m = 0.3111, Omega_L = 0.6889, Omega_b = 0.0490, h = 0.6766, ns = 0.9665, sigma8 = 0.8102)
    Used to build initial conditions with music2 (Section 2). All conclusions about halo abundances and galaxy properties are conditional on this cosmology.
  • domain assumption Haardt and Madau (2012) UV background and Cloudy cooling tables (Shen et al. 2010, 2013) accurately describe cooling and heating, with metal cooling in photo-ionization equilibrium and no self-shielding
    The cooling model is central to the multiphase ISM the paper highlights; the non-equilibrium treatment is applied only to primordial species (Section 2).
  • ad hoc to paper Stochastic subgrid star formation with a Kroupa IMF and blastwave supernova feedback, without photoionizing radiation, radiation pressure, or AGN feedback, is an adequate description of unresolved stellar feedback at z > 8
    The paper's central interpretation, that weak feedback permits rapid assembly, assumes the neglected feedback channels are unimportant at z > 8. Section 4 explicitly calls for radiative transfer calculations to test this.
  • ad hoc to paper The offset between simulated half-mass radii and observed effective radii is dominated by the roughly 25 percent half-light to half-mass offset plus resolution-driven size inflation, and is approximately mass-independent
    Used to shift the observed Yang et al. (2025) relation's y-intercept and then claim slope agreement (Section 3.1, Figure 6). Supported qualitatively by GigaEris and MassiveBlackPS, but not by a converged resolution series of stellar sizes in Phoebos itself.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Introducing the Phoebos simulation: galaxy properties at the dawn of galaxy formation." pith.science (2026). https://pith.science/paper/HBKWAFWI

@misc{pith2026250704927,
  author       = {Pith},
  title        = {Pith review of: Introducing the Phoebos simulation: galaxy properties at the dawn of galaxy formation},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/HBKWAFWI}},
  note         = {Machine review of arXiv:2507.04927}
}
abstract

The James Webb Space Telescope (JWST) now allows us to observe galaxies at the end of cosmic dawn ($z \sim 10-15$) with unprecedented detail, revealing their morphologies, sizes, and internal structures. These observations offer crucial insights into the physical processes driving early galaxy formation. In this work, we introduce the Phoebos hydrodynamical cosmological simulation, a state-of-the-art 100 Mpc volume designed to study the formation and evolution of galaxies at the end of cosmic dawn and into the epoch of reionization. Phoebos includes a stellar feedback model that is intentionally weak, in order to address the high abundance of massive galaxies seen by JWST at early epochs. At variance with most large cosmological hydrodynamical simulations, we do not employ an effective equation of state model, instead our radiative cooling model allows us to capture the multi-phase nature of the gas inside and around galaxies. Phoebos reproduces key observables of early galaxy formation at $z \gtrsim 8$, including the stellar mass function and the stellar-to-halo mass relation. It also recovers the observed slope of the stellar size-to-mass relation and matches the specific star formation rate remarkably well. These results suggest that highly efficient star formation in the presence of only mild regulation from stellar feedback, drives early galaxy growth, supporting a scenario of rapid stellar mass assembly during cosmic dawn. There are indications in the cosmic star formation density that, at lower redshifts, Phoebos might overpredict the stellar mass within the systems, suggesting that a transition to a stronger stellar feedback may be necessary to reproduce later-time observations. These results highlight the potential of Phoebos to interpret JWST observations and to probe the evolving physical processes that shape galaxy formation.

Figures

Figures reproduced from arXiv: 2507.04927 by the authors.

Figure 1
Figure 1. Baryonic mass resolution and box size for several cosmo￾logical hydrodynamical simulations from the recent literature: Il￾lustris (e.g. Sijacki et al. 2015), Magneticum (Hirschmann et al. 2014), Eagle (Schaye et al. 2015), Romulus25 (Tremmel et al. 2017), MUFASA (Davé et al. 2016), FABLE (Henden et al. 2018), Simba100 (Davé et al. 2019), FIREbox (Feldmann et al. 2023), MilleniumTNG (e.g. Hernández-Aguayo et al. 2023… view at source ↗
Figure 2
Figure 2. General properties of the Phoebos simulation. The top-left panel shows the temporal evolution of the cosmic SFRD, whereas all other panels show quantities at z = 8: the galaxy stellar mass function (top-centre panel), the total halo mass function (top-right panel), the sizes of galaxies as a function of stellar mass (bottom-left panel), the gas fraction of haloes as a function of the total halo mass, with the gray d… view at source ↗
Figure 3
Figure 3. Spin parameter distribution of our simulated galaxies at z = 8. The black dashed line indicates the peak of the distribution, which is consistent with the expected value from Bullock et al. (2001), shown for comparison as the black dotted line. Universe [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figures from the paper (12 more)
Figure 4
Figure 4. Figure 4: Total halo mass (top panel) and stellar mass (bottom panel) functions of the Phoebos simulation across different red￾shifts: z = 8 (orange solid line), 10 (brown dashed line), and 12 (red dotted line). The bottom panel also shows the observed stellar mass function from…
Figure 5
Figure 5. Figure 5: Evolution of stellar properties from z = 12 to z = 8. The top panels correspond to z = 8, whereas the bottom panels represent z = 12. The left-hand panels show histograms of the stellar half-mass radius. The right-hand panels present the stellar mass distributions. The…
Figure 6
Figure 6. Figure 6: Stellar size–mass relation at z = 8 and 12, defined be￾tween the stellar half-mass radius and the stellar mass enclosed within twice that radius. The open circles and error bars repre￾sent the median and 1σ scatter of halo sizes from Phoebos. These results are compared…
Figure 7
Figure 7. Figure 7: Stellar density evolution of the stellar component within haloes from z = 12 to z = 8. The top panel shows the correla￾tion between the stellar half-mass radius and the stellar surface density, ΣM⋆ . Simulation results are compared with observational constraints from M…
Figure 8
Figure 8. Figure 8: The stellar-to-halo mass relation (SHMR; orange solid line) and associated 1σ scatter (orange-shaded region) for galaxies in the Phoebos simulation at z = 8 (left-hand panel), z = 10 (middle panel), and z = 12 (right-hand panel). Observational constraints are overlaid …
Figure 9
Figure 9. Figure 9: Surface density maps showing the evolution of a massive halo from z ∼ 12 and z ∼ 8 in the Phoebos simulation. Rows show from top to bottom: DM surface density, gas surface density, and stellar surface density overlaid on the same gas map of the second row. The halo sho…
Figure 11
Figure 11. Figure 11: The SFR within the virial radius of the massive halo depicted in Figures 9 and 10. The vertical dashed lines mark the redshifts corresponding to the snapshots presented in the surface density maps of the same figures. For comparison, light orange lines in the backgrou…
Figure 10
Figure 10. Figure 10: Zoom in of the gas surface density maps showing the evolution of the massive halo from z ∼ 12 and z ∼ 8 of [PITH_FULL_IMAGE:figures/full_fig_p012_10.png]
Figure 12
Figure 12. Figure 12: The SF main sequence of galaxies in Phoebos at z = 8, 10, and 12, from left to right, shown by the orange hexagrams. The gray diamonds correspond to observations in the redshift range 7.5 ≲ z ≲ 8.5, 9.5 ≲ z ≲ 10.5, and 11.5 ≲ z ≲ 12.5 found by Morishita et al. (2024).…
Figure 13
Figure 13. Figure 13: The normalized sSFR distribution at z = 8, 10 and 12 from top to bottom. The gray lines indicate the observed sSFR distribution in the redshift range 7.5 ≲ z ≲ 8.5, 9.5 ≲ z ≲ 10.5 and 11.5 ≲ z ≲ 12.5 by Morishita et al. (2024). The blue vertical dashed line in each pa…
Figure 14
Figure 14. Figure 14: Gas volume density (left-hand panels) and HI volume density (right-hand panels) maps at z = 8, shown alongside the stellar density distribution. The top panels display the full stellar population, while the bottom panels focus on the subset of young stars with ages < …
Figure 15
Figure 15. Figure 15: The stellar mass-HI gas fraction relation at z = 8. The open circles and error bars represent the median and 1σ scat￾ter of the HI gas fraction of galaxies in Phoebos. These results are compared to observational data from Scholte et al. (2024) for local galaxies with …

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

196 extracted references · 10 canonical work pages

  1. [1]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...

  2. [2]

    ALMA Partnership et al., 2015, @doi [ ] 10.1088/2041-8205/808/1/L4 , https://ui.adsabs.harvard.edu/abs/2015ApJ...808L...4A 808, L4

    doi:10.1088/2041-8205/808/1/l4 2015

  3. [3]

    J., et al., 2024, @doi [ ] 10.3847/1538-4357/ad2a7b , https://ui.adsabs.harvard.edu/abs/2024ApJ...965..169A 965, 169

    Adams N. J., et al., 2024, @doi [ ] 10.3847/1538-4357/ad2a7b , https://ui.adsabs.harvard.edu/abs/2024ApJ...965..169A 965, 169

    doi:10.3847/1538-4357/ad2a7b 2024

  4. [4]

    J., et al., 2017, @doi [ ] 10.3847/2041-8213/834/2/L11 , https://ui.adsabs.harvard.edu/abs/2017ApJ...834L..11A 834, L11

    Allen R. J., et al., 2017, @doi [ ] 10.3847/2041-8213/834/2/L11 , https://ui.adsabs.harvard.edu/abs/2017ApJ...834L..11A 834, L11

    doi:10.3847/2041-8213/834/2/l11 2017

  5. [5]

    Anderson L., Governato F., Karcher M., Quinn T., Wadsley J., 2017, @doi [ ] 10.1093/mnras/stx709 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.468.4077A 468, 4077

    doi:10.1093/mnras/stx709 2017

  6. [6]

    Bacchini C., Fraternali F., Iorio G., Pezzulli G., Marasco A., Nipoti C., 2020, @doi [ ] 10.1051/0004-6361/202038223 , https://ui.adsabs.harvard.edu/abs/2020A&A...641A..70B 641, A70

    doi:10.1051/0004-6361/202038223 2020

  7. [7]

    Baggen J. F. W., et al., 2023, @doi [ ] 10.3847/2041-8213/acf5ef , https://ui.adsabs.harvard.edu/abs/2023ApJ...955L..12B 955, L12

    doi:10.3847/2041-8213/acf5ef 2023

  8. [8]

    Barrow K. S. S., Wise J. H., Norman M. L., O'Shea B. W., Xu H., 2017, @doi [ ] 10.1093/mnras/stx1181 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.469.4863B 469, 4863

    doi:10.1093/mnras/stx1181 2017

Show all 196 references
  1. [9]

    R., Burkert A., 1997, @doi [ ] 10.1093/mnras/288.4.1060 , https://ui.adsabs.harvard.edu/abs/1997MNRAS.288.1060B 288, 1060

    Bate M. R., Burkert A., 1997, @doi [ ] 10.1093/mnras/288.4.1060 , https://ui.adsabs.harvard.edu/abs/1997MNRAS.288.1060B 288, 1060

    1997 doi

  2. [10]

    H., Hearin A

    Behroozi P., Wechsler R. H., Hearin A. P., Conroy C., 2019, @doi [ ] 10.1093/mnras/stz1182 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.488.3143B 488, 3143

    2019 doi

  3. [11]

    G., Tal T., Marchesini D., Kriek M., Franx M., Coppi P., 2009, @doi [ ] 10.1088/0004-637X/697/2/1290 , https://ui.adsabs.harvard.edu/abs/2009ApJ...697.1290B 697, 1290

    Bezanson R., van Dokkum P. G., Tal T., Marchesini D., Kriek M., Franx M., Coppi P., 2009, @doi [ ] 10.1088/0004-637X/697/2/1290 , https://ui.adsabs.harvard.edu/abs/2009ApJ...697.1290B 697, 1290

    2009 doi

  4. [12]

    A., Fraternali F., van der Hulst J

    Boomsma R., Oosterloo T. A., Fraternali F., van der Hulst J. M., Sancisi R., 2008, @doi [ ] 10.1051/0004-6361:200810120 , https://ui.adsabs.harvard.edu/abs/2008A&A...490..555B 490, 555

    2008 doi

  5. [13]

    J., Illingworth G

    Bouwens R. J., Illingworth G. D., van Dokkum P. G., Oesch P. A., Stefanon M., Ribeiro B., 2022, @doi [ ] 10.3847/1538-4357/ac4791 , https://ui.adsabs.harvard.edu/abs/2022ApJ...927...81B 927, 81

    2022 doi

  6. [14]

    J., et al., 2023, @doi [ ] 10.1093/mnras/stad1145 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.523.1036B 523, 1036

    Bouwens R. J., et al., 2023, @doi [ ] 10.1093/mnras/stad1145 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.523.1036B 523, 1036

    2023 doi

  7. [15]

    Boylan-Kolchin M., 2023, @doi [Nature Astronomy] 10.1038/s41550-023-01937-7 , https://ui.adsabs.harvard.edu/abs/2023NatAs...7..731B 7, 731

    2023 doi

  8. [17]

    J., Bouwens R

    Buitrago F., Trujillo I., Conselice C. J., Bouwens R. J., Dickinson M., Yan H., 2008, @doi [ ] 10.1086/592836 , https://ui.adsabs.harvard.edu/abs/2008ApJ...687L..61B 687, L61

    2008 doi

  9. [18]

    S., Dekel A., Kolatt T

    Bullock J. S., Dekel A., Kolatt T. S., Kravtsov A. V., Klypin A. A., Porciani C., Primack J. R., 2001, @doi [ ] 10.1086/321477 , https://ui.adsabs.harvard.edu/abs/2001ApJ...555..240B 555, 240

    2001 doi

  10. [19]

    D., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2502.13244 , https://ui.adsabs.harvard.edu/abs/2025arXiv250213244B p

    Burger J. D., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2502.13244 , https://ui.adsabs.harvard.edu/abs/2025arXiv250213244B p. arXiv:2502.13244

    2025 doi

  11. [20]

    Calabr \`o A., et al., 2024, @doi [ ] 10.1051/0004-6361/202449768 , https://ui.adsabs.harvard.edu/abs/2024A&A...690A.290C 690, A290

    2024 doi

  12. [21]

    R., Bovino S., Lupi A., Schleicher D

    Capelo P. R., Bovino S., Lupi A., Schleicher D. R. G., Grassi T., 2018, @doi [ ] 10.1093/mnras/stx3355 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.475.3283C 475, 3283

    2018 doi

  13. [22]

    G., Greene J

    Carlsten S. G., Greene J. E., Greco J. P., Beaton R. L., Kado-Fong E., 2021, @doi [ ] 10.3847/1538-4357/ac2581 , https://ui.adsabs.harvard.edu/abs/2021ApJ...922..267C 922, 267

    2021 doi

  14. [23]

    Catinella B., et al., 2018, @doi [ ] 10.1093/mnras/sty089 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.476..875C 476, 875

    2018 doi

  15. [24]

    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

  16. [26]

    Costantin L., et al., 2023, @doi [ ] 10.3847/1538-4357/acb926 , https://ui.adsabs.harvard.edu/abs/2023ApJ...946...71C 946, 71

    2023 doi

  17. [28]

    Daddi E., et al., 2005, @doi [ ] 10.1086/430104 , https://ui.adsabs.harvard.edu/abs/2005ApJ...626..680D 626, 680

    2005 doi

  18. [29]

    F., 2016, @doi [ ] 10.1093/mnras/stw1862 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.462.3265D 462, 3265

    Dav \'e R., Thompson R., Hopkins P. F., 2016, @doi [ ] 10.1093/mnras/stw1862 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.462.3265D 462, 3265

    2016 doi

  19. [30]

    H., Appleby S., 2019, @doi [ ] 10.1093/mnras/stz937 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.486.2827D 486, 2827

    Dav \'e R., Angl \'e s-Alc \'a zar D., Narayanan D., Li Q., Rafieferantsoa M. H., Appleby S., 2019, @doi [ ] 10.1093/mnras/stz937 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.486.2827D 486, 2827

    2019 doi

  20. [32]

    E., Nanopoulos D

    Dekel A., Birnboim Y., 2004, in Allen R. E., Nanopoulos D. V., Pope C. N., eds, American Institute of Physics Conference Series Vol. 743, The New Cosmology: Conference on Strings and Cosmology. AIP, pp 162--189, @doi 10.1063/1.1848326

    2004 doi

  21. [33]

    C., Birnboim Y., Mandelker N., Li Z., 2023, @doi [ ] 10.1093/mnras/stad1557 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.523.3201D 523, 3201

    Dekel A., Sarkar K. C., Birnboim Y., Mandelker N., Li Z., 2023, @doi [ ] 10.1093/mnras/stad1557 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.523.3201D 523, 3201

    2023 doi

  22. [34]

    C., Dutta Chowdhury D., Gilbaum S., Li Z., Mandelker N., van den Bosch F

    Dekel A., Stone N. C., Dutta Chowdhury D., Gilbaum S., Li Z., Mandelker N., van den Bosch F. C., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2409.18605 , https://ui.adsabs.harvard.edu/abs/2024arXiv240918605D p. arXiv:2409.18605

    2024 doi arXiv

  23. [35]

    Dubois Y., et al., 2014, @doi [ ] 10.1093/mnras/stu1227 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.444.1453D 444, 1453

    2014 doi

  24. [36]

    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

  25. [37]

    J., Hu W., 1998, @doi [ ] 10.1086/305424 , https://ui.adsabs.harvard.edu/abs/1998ApJ...496..605E 496, 605

    Eisenstein D. J., Hu W., 1998, @doi [ ] 10.1086/305424 , https://ui.adsabs.harvard.edu/abs/1998ApJ...496..605E 496, 605

    1998 doi

  26. [38]

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

    2023 doi

  27. [39]

    A., Bird S., Battaglia N., Wilkins S., 2016, @doi [ ] 10.1093/mnras/stv2484 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.455.2778F 455, 2778

    Feng Y., Di-Matteo T., Croft R. A., Bird S., Battaglia N., Wilkins S., 2016, @doi [ ] 10.1093/mnras/stv2484 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.455.2778F 455, 2778

    2016 doi

  28. [40]

    J., Korista K

    Ferland G. J., Korista K. T., Verner D. A., Ferguson J. W., Kingdon J. B., Verner E. M., 1998, @doi [ ] 10.1086/316190 , https://ui.adsabs.harvard.edu/abs/1998PASP..110..761F 110, 761

    1998 doi

  29. [41]

    J., et al., 2013, @doi [ ] 10.48550/arXiv.1302.4485 , https://ui.adsabs.harvard.edu/abs/2013RMxAA..49..137F 49, 137

    Ferland G. J., et al., 2013, @doi [ ] 10.48550/arXiv.1302.4485 , https://ui.adsabs.harvard.edu/abs/2013RMxAA..49..137F 49, 137

    2013 doi arXiv

  30. [42]

    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

  31. [43]

    Ferreira L., et al., 2022, @doi [ ] 10.3847/2041-8213/ac947c , https://ui.adsabs.harvard.edu/abs/2022ApJ...938L...2F 938, L2

    2022 doi

  32. [44]

    Fiacconi D., Mayer L., Madau P., Lupi A., Dotti M., Haardt F., 2017, @doi [ ] 10.1093/mnras/stx335 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.467.4080F 467, 4080

    2017 doi

  33. [45]

    Fumagalli M., Gavazzi G., 2008, @doi [ ] 10.1051/0004-6361:200810604 , https://ui.adsabs.harvard.edu/abs/2008A&A...490..571F 490, 571

    2008 doi

  34. [46]

    P., et al., 2006, @doi [ ] 10.1007/s11214-006-8315-7 , https://ui.adsabs.harvard.edu/abs/2006SSRv..123..485G 123, 485

    Gardner J. P., et al., 2006, @doi [ ] 10.1007/s11214-006-8315-7 , https://ui.adsabs.harvard.edu/abs/2006SSRv..123..485G 123, 485

    2006 doi

  35. [47]

    Gensior J., et al., 2024, @doi [ ] 10.1093/mnras/stae1217 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.531.1158G 531, 1158

    2024 doi

  36. [48]

    Gill S. P. D., Knebe A., Gibson B. K., 2004, @doi [ ] 10.1111/j.1365-2966.2004.07786.x , https://ui.adsabs.harvard.edu/abs/2004MNRAS.351..399G 351, 399

    2004

  37. [49]

    Gross M. A. K., 1997, PhD thesis, University of California, Santa Cruz

    1997

  38. [50]

    Guedes J., Callegari S., Madau P., Mayer L., 2011, @doi [ ] 10.1088/0004-637X/742/2/76 , https://ui.adsabs.harvard.edu/abs/2011ApJ...742...76G 742, 76

    2011 doi

  39. [51]

    Haardt F., Madau P., 2012, @doi [ ] 10.1088/0004-637X/746/2/125 , https://ui.adsabs.harvard.edu/abs/2012ApJ...746..125H 746, 125

    2012 doi

  40. [52]

    Hahn O., Abel T., 2011, @doi [ ] 10.1111/j.1365-2966.2011.18820.x , https://ui.adsabs.harvard.edu/abs/2011MNRAS.415.2101H 415, 2101

    2011

  41. [53]

    Hahn O., Rampf C., Uhlemann C., 2021, @doi [ ] 10.1093/mnras/staa3773 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.503..426H 503, 426

    2021 doi

  42. [54]

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

    2023 doi

  43. [55]

    Harikane Y., Nakajima K., Ouchi M., Umeda H., Isobe Y., Ono Y., Xu Y., Zhang Y., 2024, @doi [ ] 10.3847/1538-4357/ad0b7e , https://ui.adsabs.harvard.edu/abs/2024ApJ...960...56H 960, 56

    2024 doi

  44. [56]

    Harvey T., et al., 2025, @doi [ ] 10.3847/1538-4357/ad8c29 , https://ui.adsabs.harvard.edu/abs/2025ApJ...978...89H 978, 89

    2025 doi

  45. [57]

    A., Puchwein E., Shen S., Sijacki D., 2018, @doi [ ] 10.1093/mnras/sty1780 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.479.5385H 479, 5385

    Henden N. A., Puchwein E., Shen S., Sijacki D., 2018, @doi [ ] 10.1093/mnras/sty1780 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.479.5385H 479, 5385

    2018 doi

  46. [58]

    Hern \'a ndez-Aguayo C., et al., 2023, @doi [ ] 10.1093/mnras/stad1657 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.524.2556H 524, 2556

    2023 doi

  47. [59]

    Hirschmann M., Dolag K., Saro A., Bachmann L., Borgani S., Burkert A., 2014, @doi [ ] 10.1093/mnras/stu1023 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.442.2304H 442, 2304

    2014 doi

  48. [61]

    F., Kere s D., O \ n orbe J., Faucher-Gigu \`e re C.-A., Quataert E., Murray N., Bullock J

    Hopkins P. F., Kere s D., O \ n orbe J., Faucher-Gigu \`e re C.-A., Quataert E., Murray N., Bullock J. S., 2014, @doi [ ] 10.1093/mnras/stu1738 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.445..581H 445, 581

    2014 doi

  49. [62]

    F., et al., 2018, @doi [ ] 10.1093/mnras/sty1690 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.480..800H 480, 800

    Hopkins P. F., et al., 2018, @doi [ ] 10.1093/mnras/sty1690 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.480..800H 480, 800

    2018 doi

  50. [63]

    arXiv:2305.02478

    Huertas-Company M., et al., 2023, @doi [arXiv e-prints] 10.48550/arXiv.2305.02478 , https://ui.adsabs.harvard.edu/abs/2023arXiv230502478H p. arXiv:2305.02478

    2023 doi arXiv

  51. [64]

    M., Cortese L., Boselli A., Gavazzi G., Davies J

    Hughes T. M., Cortese L., Boselli A., Gavazzi G., Davies J. I., 2013, @doi [ ] 10.1051/0004-6361/201218822 , https://ui.adsabs.harvard.edu/abs/2013A&A...550A.115H 550, A115

    2013 doi

  52. [65]

    Ito K., et al., 2024, @doi [ ] 10.3847/1538-4357/ad2512 , https://ui.adsabs.harvard.edu/abs/2024ApJ...964..192I 964, 192

    2024 doi

  53. [66]

    Jarvis M., et al., 2016, in MeerKAT Science: On the Pathway to the SKA. p. 6 ( @eprint arXiv 1709.01901 ), @doi 10.22323/1.277.0006

    2016 arXiv

  54. [67]

    H., 1902, @doi [Philosophical Transactions of the Royal Society of London Series A] 10.1098/rsta.1902.0012 , https://ui.adsabs.harvard.edu/abs/1902RSPTA.199....1J 199, 1

    Jeans J. H., 1902, @doi [Philosophical Transactions of the Royal Society of London Series A] 10.1098/rsta.1902.0012 , https://ui.adsabs.harvard.edu/abs/1902RSPTA.199....1J 199, 1

    1902

  55. [68]

    V., Quinn T., 2008, in 2008 IEEE International Symposium on Parallel and Distributed Processing

    Jetley P., Gioachin F., Mendes C., Kale L. V., Quinn T., 2008, in 2008 IEEE International Symposium on Parallel and Distributed Processing. pp 1--12, @doi 10.1109/IPDPS.2008.4536319

    2008

  56. [69]

    V., Quinn T

    Jetley P., Wesolowski L., Gioachin F., Kalé L. V., Quinn T. R., 2010, in SC '10: Proceedings of the 2010 ACM/IEEE International Conference for High Performance Computing, Networking, Storage and Analysis. pp 1--11, @doi 10.1109/SC.2010.49

    2010 doi

  57. [70]

    P., Koncz B., Pinter S., T \'o th L

    Jo \'o A. P., Koncz B., Pinter S., T \'o th L. V., 2023, in Wong T., Kim W.-T., eds, IAU Symposium Vol. 373, Resolving the Rise and Fall of Star Formation in Galaxies. pp 318--321, @doi 10.1017/S1743921323000157

    2023 doi

  58. [71]

    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

  59. [72]

    arXiv:2502.20437

    Kannan R., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2502.20437 , https://ui.adsabs.harvard.edu/abs/2025arXiv250220437K p. arXiv:2502.20437

    2025 doi

  60. [73]

    S., et al., 2023, @doi [ ] 10.3847/2041-8213/acad01 , https://ui.adsabs.harvard.edu/abs/2023ApJ...946L..15K 946, L15

    Kartaltepe J. S., et al., 2023, @doi [ ] 10.3847/2041-8213/acad01 , https://ui.adsabs.harvard.edu/abs/2023ApJ...946L..15K 946, L15

    2023 doi

  61. [74]

    Katz N., 1992, @doi [ ] 10.1086/171366 , https://ui.adsabs.harvard.edu/abs/1992ApJ...391..502K 391, 502

    1992 doi

  62. [75]

    Kaviraj S., et al., 2017, @doi [ ] 10.1093/mnras/stx126 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.467.4739K 467, 4739

    2017 doi

  63. [76]

    Kawamata R., Ishigaki M., Shimasaku K., Oguri M., Ouchi M., 2015, @doi [ ] 10.1088/0004-637X/804/2/103 , https://ui.adsabs.harvard.edu/abs/2015ApJ...804..103K 804, 103

    2015 doi

  64. [77]

    Kawamata R., Ishigaki M., Shimasaku K., Oguri M., Ouchi M., Tanigawa S., 2018, @doi [ ] 10.3847/1538-4357/aaa6cf , https://ui.adsabs.harvard.edu/abs/2018ApJ...855....4K 855, 4

    2018 doi

  65. [78]

    Kennicutt Jr. R. C., 1989, @doi [ ] 10.1086/167834 , https://ui.adsabs.harvard.edu/abs/1989ApJ...344..685K 344, 685

    1989 doi

  66. [79]

    Kennicutt Jr. R. C., 1998, @doi [ ] 10.1086/305588 , https://ui.adsabs.harvard.edu/abs/1998ApJ...498..541K 498, 541

    1998 doi

  67. [80]

    Kennicutt Jr. R. C., Tamblyn P., Congdon C. E., 1994, @doi [ ] 10.1086/174790 , https://ui.adsabs.harvard.edu/abs/1994ApJ...435...22K 435, 22

    1994 doi

  68. [81]

    Kim J.-h., et al., 2016, @doi [ ] 10.3847/1538-4357/833/2/202 , https://ui.adsabs.harvard.edu/abs/2016ApJ...833..202K 833, 202

    2016 doi

  69. [82]

    R., Knebe A., 2009, @doi [ ] 10.1088/0067-0049/182/2/608 , https://ui.adsabs.harvard.edu/abs/2009ApJS..182..608K 182, 608

    Knollmann S. R., Knebe A., 2009, @doi [ ] 10.1088/0067-0049/182/2/608 , https://ui.adsabs.harvard.edu/abs/2009ApJS..182..608K 182, 608

    2009 doi

  70. [83]

    M., et al., 2011, @doi [ ] 10.1088/0067-0049/197/2/36 , https://ui.adsabs.harvard.edu/abs/2011ApJS..197...36K 197, 36

    Koekemoer A. M., et al., 2011, @doi [ ] 10.1088/0067-0049/197/2/36 , https://ui.adsabs.harvard.edu/abs/2011ApJS..197...36K 197, 36

    2011 doi

  71. [84]

    Kohandel M., Pallottini A., Ferrara A., Zanella A., Rizzo F., Carniani S., 2024, @doi [ ] 10.1051/0004-6361/202348209 , https://ui.adsabs.harvard.edu/abs/2024A&A...685A..72K 685, A72

    2024 doi

  72. [85]

    S., et al., 2020, @doi [ ] 10.1007/s10509-020-03831-4 , https://ui.adsabs.harvard.edu/abs/2020Ap&SS.365..118K 365, 118

    Koribalski B. S., et al., 2020, @doi [ ] 10.1007/s10509-020-03831-4 , https://ui.adsabs.harvard.edu/abs/2020Ap&SS.365..118K 365, 118

    2020 doi

  73. [86]

    V., 2013, @doi [ ] 10.1088/2041-8205/764/2/L31 , https://ui.adsabs.harvard.edu/abs/2013ApJ...764L..31K 764, L31

    Kravtsov A. V., 2013, @doi [ ] 10.1088/2041-8205/764/2/L31 , https://ui.adsabs.harvard.edu/abs/2013ApJ...764L..31K 764, L31

    2013 doi

  74. [87]

    Kretschmer M., Dekel A., Teyssier R., 2022, @doi [ ] 10.1093/mnras/stab3648 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.510.3266K 510, 3266

    2022 doi

  75. [88]

    Kroupa P., 2001, @doi [ ] 10.1046/j.1365-8711.2001.04022.x , https://ui.adsabs.harvard.edu/abs/2001MNRAS.322..231K 322, 231

    2001

  76. [89]

    arXiv:2401.16608

    LaChance P., Croft R., Ni Y., Chen N., Di Matteo T., Bird S., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2401.16608 , https://ui.adsabs.harvard.edu/abs/2024arXiv240116608L p. arXiv:2401.16608

    2024 doi arXiv

  77. [90]

    Lange R., et al., 2015, @doi [ ] 10.1093/mnras/stu2467 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.447.2603L 447, 2603

    2015 doi

  78. [91]

    Lee S., et al., 2025, @doi [Publications of the Astronomical Society of Australia] 10.1017/pasa.2025.30 , 42

    2025 doi

  79. [92]

    K., et al., 2020, @doi [ ] 10.3847/1538-4357/aba044 , https://ui.adsabs.harvard.edu/abs/2020ApJ...899...58L 899, 58

    Leslie S. K., et al., 2020, @doi [ ] 10.3847/1538-4357/aba044 , https://ui.adsabs.harvard.edu/abs/2020ApJ...899...58L 899, 58

    2020 doi

  80. [93]

    C., Aung H., Giavalisco M., Mandelker N., Tacchella S., 2024, @doi [ ] 10.1051/0004-6361/202348727 , https://ui.adsabs.harvard.edu/abs/2024A&A...690A.108L 690, A108

    Li Z., Dekel A., Sarkar K. C., Aung H., Giavalisco M., Mandelker N., Tacchella S., 2024, @doi [ ] 10.1051/0004-6361/202348727 , https://ui.adsabs.harvard.edu/abs/2024A&A...690A.108L 690, A108

    2024 doi

  81. [94]

    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

  82. [95]

    C., Harrison I., Harikane Y., Tacchella S., Wilkins S

    Lovell C. C., Harrison I., Harikane Y., Tacchella S., Wilkins S. M., 2023, @doi [ ] 10.1093/mnras/stac3224 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.518.2511L 518, 2511

    2023 doi

  83. [96]

    Ma X., et al., 2018a, @doi [ ] 10.1093/mnras/sty684 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.477..219M 477, 219

    doi

  84. [97]

    Ma X., et al., 2018b, @doi [ ] 10.1093/mnras/sty1024 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.478.1694M 478, 1694

    doi

  85. [98]

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

    2018 doi

  86. [99]

    A., Wilkins S., Di Matteo T., Roper W

    Marshall M. A., Wilkins S., Di Matteo T., Roper W. J., Vijayan A. P., Ni Y., Feng Y., Croft R. A. C., 2022, @doi [ ] 10.1093/mnras/stac380 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.511.5475M 511, 5475

    2022 doi

  87. [100]

    R., Zwick L., Di Matteo T., 2024, @doi [ ] 10.3847/1538-4357/ad11cf , https://ui.adsabs.harvard.edu/abs/2024ApJ...961...76M 961, 76

    Mayer L., Capelo P. R., Zwick L., Di Matteo T., 2024, @doi [ ] 10.3847/1538-4357/ad11cf , https://ui.adsabs.harvard.edu/abs/2024ApJ...961...76M 961, 76

    2024 doi

  88. [101]

    R., Adamo A., 2025, @doi [ ] 10.3847/2041-8213/adadfe , https://ui.adsabs.harvard.edu/abs/2025ApJ...981L..28M 981, L28

    Mayer L., van Donkelaar F., Messa M., Capelo P. R., Adamo A., 2025, @doi [ ] 10.3847/2041-8213/adadfe , https://ui.adsabs.harvard.edu/abs/2025ApJ...981L..28M 981, L28

    2025 doi

  89. [102]

    F., Ostriker J

    McKee C. F., Ostriker J. P., 1977, @doi [ ] 10.1086/155667 , https://ui.adsabs.harvard.edu/abs/1977ApJ...218..148M 218, 148

    1977 doi

  90. [103]

    Menon H., Wesolowski L., Zheng G., Jetley P., Kale L., Quinn T., Governato F., 2015, @doi [Computational Astrophysics and Cosmology] 10.1186/s40668-015-0007-9 , https://ui.adsabs.harvard.edu/abs/2015ComAC...2....1M 2, 1

    2015 doi

  91. [104]

    Merlin E., et al., 2019, @doi [ ] 10.1093/mnras/stz2615 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.490.3309M 490, 3309

    2019 doi

  92. [105]

    E., 2021, @doi [ ] 10.1093/mnras/staa3149 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.500..663M 500, 663

    Michaux M., Hahn O., Rampf C., Angulo R. E., 2021, @doi [ ] 10.1093/mnras/staa3149 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.500..663M 500, 663

    2021 doi

  93. [106]

    B., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2412.06957 , https://ui.adsabs.harvard.edu/abs/2024arXiv241206957M p

    Miller T. B., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2412.06957 , https://ui.adsabs.harvard.edu/abs/2024arXiv241206957M p. arXiv:2412.06957

    2024 doi arXiv

  94. [107]

    J., Mao S., White S

    Mo H. J., Mao S., White S. D. M., 1998, @doi [ ] 10.1046/j.1365-8711.1998.01227.x , https://ui.adsabs.harvard.edu/abs/1998MNRAS.295..319M 295, 319

    1998

  95. [108]

    Morishita T., Ichikawa T., Kajisawa M., 2014, @doi [ ] 10.1088/0004-637X/785/1/18 , https://ui.adsabs.harvard.edu/abs/2014ApJ...785...18M 785, 18

    2014 doi

  96. [109]

    Morishita T., et al., 2024, @doi [ ] 10.3847/1538-4357/ad1404 , https://ui.adsabs.harvard.edu/abs/2024ApJ...963....9M 963, 9

    2024 doi

  97. [110]

    Mosleh M., et al., 2012, @doi [ ] 10.1088/2041-8205/756/1/L12 , https://ui.adsabs.harvard.edu/abs/2012ApJ...756L..12M 756, L12

    2012 doi

  98. [111]

    Z., Tacchella S., 2020, @doi [ ] 10.3847/1538-4357/abc7cc , https://ui.adsabs.harvard.edu/abs/2020ApJ...905..170M 905, 170

    Mosleh M., Hosseinnejad S., Hosseini-ShahiSavandi S. Z., Tacchella S., 2020, @doi [ ] 10.3847/1538-4357/abc7cc , https://ui.adsabs.harvard.edu/abs/2020ApJ...905..170M 905, 170

    2020 doi

  99. [112]

    A., et al., 2019, @doi [ ] 10.3847/1538-4357/ab290a , https://ui.adsabs.harvard.edu/abs/2019ApJ...880...57M 880, 57

    Mowla L. A., et al., 2019, @doi [ ] 10.3847/1538-4357/ab290a , https://ui.adsabs.harvard.edu/abs/2019ApJ...880...57M 880, 57

    2019 doi

  100. [113]

    Munshi F., et al., 2013, @doi [ ] 10.1088/0004-637X/766/1/56 , https://ui.adsabs.harvard.edu/abs/2013ApJ...766...56M 766, 56

    2013 doi

  101. [114]

    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

  102. [115]

    Nakazato Y., Ceverino D., Yoshida N., 2024, @doi [ ] 10.3847/1538-4357/ad7d0b , https://ui.adsabs.harvard.edu/abs/2024ApJ...975..238N 975, 238

    2024 doi

  103. [116]

    V., et al., 2021, @doi [ ] 10.1093/mnras/stab1744 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.506..928N 506, 928

    Nedkova K. V., et al., 2021, @doi [ ] 10.1093/mnras/stab1744 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.506..928N 506, 928

    2021 doi

  104. [117]

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

    2018 doi

  105. [118]

    Nelson D., et al., 2019, @doi [ ] 10.1093/mnras/stz2306 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.490.3234N 490, 3234

    2019 doi

  106. [119]

    arXiv:2505.04299

    O'Beirne T., et al., 2025, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2025arXiv250504299O p. arXiv:2505.04299

    2025 arXiv

  107. [120]

    A., et al., 2010, @doi [ ] 10.1088/2041-8205/709/1/L21 , https://ui.adsabs.harvard.edu/abs/2010ApJ...709L..21O 709, L21

    Oesch P. A., et al., 2010, @doi [ ] 10.1088/2041-8205/709/1/L21 , https://ui.adsabs.harvard.edu/abs/2010ApJ...709L..21O 709, L21

    2010 doi

  108. [121]

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

    2024 doi

  109. [122]

    Ono Y., et al., 2013, @doi [ ] 10.1088/0004-637X/777/2/155 , https://ui.adsabs.harvard.edu/abs/2013ApJ...777..155O 777, 155

    2013 doi

  110. [123]

    Ono Y., et al., 2023, @doi [ ] 10.3847/1538-4357/acd44a , https://ui.adsabs.harvard.edu/abs/2023ApJ...951...72O 951, 72

    2023 doi

  111. [124]

    Ormerod K., et al., 2024, @doi [ ] 10.1093/mnras/stad3597 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.527.6110O 527, 6110

    2024 doi

  112. [125]

    E., Fielding D

    Orr M. E., Fielding D. B., Hayward C. C., Burkhart B., 2022, @doi [ ] 10.3847/2041-8213/ac479f , https://ui.adsabs.harvard.edu/abs/2022ApJ...924L..28O 924, L28

    2022 doi

  113. [126]

    P., Khochfar S., Dalla C

    Paardekooper J. P., Khochfar S., Dalla C. V., 2013, @doi [ ] 10.1093/mnrasl/sls032 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.429L..94P 429, L94

    2013 doi

  114. [127]

    arXiv:2501.11674

    Paquereau L., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2501.11674 , https://ui.adsabs.harvard.edu/abs/2025arXiv250111674P p. arXiv:2501.11674

    2025 doi

  115. [128]

    C., Brandt J

    Petersen C. C., Brandt J. C., 1995, Hubble vision. Astronomy with the Hubble Space Telescope

    1995

  116. [129]

    Pforr J., Maraston C., Tonini C., 2012, @doi [ ] 10.1111/j.1365-2966.2012.20848.x , https://ui.adsabs.harvard.edu/abs/2012MNRAS.422.3285P 422, 3285

    2012

  117. [130]

    Pforr J., Maraston C., Tonini C., 2013, @doi [ ] 10.1093/mnras/stt1382 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.435.1389P 435, 1389

    2013 doi

  118. [131]

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

    2018 doi

  119. [132]

    Planck Collaboration et al., 2014, @doi [ ] 10.1051/0004-6361/201321591 , https://ui.adsabs.harvard.edu/abs/2014A&A...571A..16P 571, A16

    2014 doi

  120. [133]

    Planck Collaboration et al., 2020, @doi [ ] 10.1051/0004-6361/201833910 , https://ui.adsabs.harvard.edu/abs/2020A&A...641A...6P 641, A6

    2020 doi

  121. [134]

    Pontzen A., et al., 2008, @doi [ ] 10.1111/j.1365-2966.2008.13782.x , https://ui.adsabs.harvard.edu/abs/2008MNRAS.390.1349P 390, 1349

    2008

  122. [135]

    S., Trager S

    Popping G., Somerville R. S., Trager S. C., 2014, @doi [ ] 10.1093/mnras/stu991 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.442.2398P 442, 2398

    2014 doi

  123. [136]

    arXiv:2408.11037

    Punyasheel P., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2408.11037 , https://ui.adsabs.harvard.edu/abs/2024arXiv240811037P p. arXiv:2408.11037

    2024 doi arXiv

  124. [137]

    M., Villata M., Navarro J

    Raiteri C. M., Villata M., Navarro J. F., 1996, , https://ui.adsabs.harvard.edu/abs/1996A&A...315..105R 315, 105

    1996

  125. [138]

    Rampf C., Uhlemann C., Hahn O., 2021, @doi [ ] 10.1093/mnras/staa3605 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.503..406R 503, 406

    2021 doi

  126. [139]

    S., Smith R

    Reed D. S., Smith R. E., Potter D., Schneider A., Stadel J., Moore B., 2013, @doi [ ] 10.1093/mnras/stt301 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.431.1866R 431, 1866

    2013 doi

  127. [140]

    P., Stacey H

    Rizzo F., Vegetti S., Powell D., Fraternali F., McKean J. P., Stacey H. R., White S. D. M., 2020, @doi [ ] 10.1038/s41586-020-2572-6 , https://ui.adsabs.harvard.edu/abs/2020Natur.584..201R 584, 201

    2020 doi

  128. [141]

    R., Powell D., 2021, @doi [ ] 10.1093/mnras/stab2295 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.507.3952R 507, 3952

    Rizzo F., Vegetti S., Fraternali F., Stacey H. R., Powell D., 2021, @doi [ ] 10.1093/mnras/stab2295 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.507.3952R 507, 3952

    2021 doi

  129. [142]

    E., et al., 2023, @doi [ ] 10.3847/2041-8213/aca086 , https://ui.adsabs.harvard.edu/abs/2023ApJ...942L..42R 942, L42

    Robertson B. E., et al., 2023, @doi [ ] 10.3847/2041-8213/aca086 , https://ui.adsabs.harvard.edu/abs/2023ApJ...942L..42R 942, L42

    2023 doi

  130. [143]

    Robertson B., et al., 2024, @doi [ ] 10.3847/1538-4357/ad463d , https://ui.adsabs.harvard.edu/abs/2024ApJ...970...31R 970, 31

    2024 doi

  131. [144]

    Roman-Oliveira F., Fraternali F., Rizzo F., 2023, @doi [ ] 10.1093/mnras/stad530 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.521.1045R 521, 1045

    2023 doi

  132. [145]

    J., Lovell C

    Roper W. J., Lovell C. C., Vijayan A. P., Marshall M. A., Irodotou D., Kuusisto J. K., Thomas P. A., Wilkins S. M., 2022, @doi [ ] 10.1093/mnras/stac1368 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.514.1921R 514, 1921

    2022 doi

  133. [146]

    J., et al., 2023, @doi [ ] 10.1093/mnras/stad2746 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.526.6128R 526, 6128

    Roper W. J., et al., 2023, @doi [ ] 10.1093/mnras/stad2746 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.526.6128R 526, 6128

    2023 doi

  134. [147]

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

    2018 doi

  135. [148]

    Saintonge A., Catinella B., 2022, @doi [ ] 10.1146/annurev-astro-021022-043545 , https://ui.adsabs.harvard.edu/abs/2022ARA&A..60..319S 60, 319

    2022 doi

  136. [149]

    Schaye J., et al., 2010, @doi [ ] 10.1111/j.1365-2966.2009.16029.x , https://ui.adsabs.harvard.edu/abs/2010MNRAS.402.1536S 402, 1536

    2010

  137. [150]

    Schaye J., et al., 2015, @doi [ ] 10.1093/mnras/stu2058 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.446..521S 446, 521

    2015 doi

  138. [151]

    Schaye J., et al., 2023, @doi [ ] 10.1093/mnras/stad2419 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.526.4978S 526, 4978

    2023 doi

  139. [152]

    Schmidt M., 1959, @doi [ ] 10.1086/146614 , https://ui.adsabs.harvard.edu/abs/1959ApJ...129..243S 129, 243

    1959 doi

  140. [153]

    Schmidt M., 1963, @doi [ ] 10.1086/147553 , https://ui.adsabs.harvard.edu/abs/1963ApJ...137..758S 137, 758

    1963 doi

  141. [154]

    Scholte D., et al., 2024, @doi [ ] 10.1093/mnras/stae2477 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.535.2341S 535, 2341

    2024 doi

  142. [155]

    Scoccimarro R., 1998, , http://esoads.eso.org/abs/1998MNRAS.299.1097S 299, 1097

    1998

  143. [156]

    Shen S., Wadsley J., Stinson G., 2010, @doi [ ] 10.1111/j.1365-2966.2010.17047.x , https://ui.adsabs.harvard.edu/abs/2010MNRAS.407.1581S 407, 1581

    2010

  144. [157]

    X., Wadsley J., 2013, @doi [ ] 10.1088/0004-637X/765/2/89 , https://ui.adsabs.harvard.edu/abs/2013ApJ...765...89S 765, 89

    Shen S., Madau P., Guedes J., Mayer L., Prochaska J. X., Wadsley J., 2013, @doi [ ] 10.1088/0004-637X/765/2/89 , https://ui.adsabs.harvard.edu/abs/2013ApJ...765...89S 765, 89

    2013 doi

  145. [158]

    arXiv:2402.08717

    Shen X., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2402.08717 , https://ui.adsabs.harvard.edu/abs/2024arXiv240208717S p. arXiv:2402.08717

    2024 doi arXiv

  146. [159]

    Shibuya T., Ouchi M., Harikane Y., 2015, @doi [ ] 10.1088/0067-0049/219/2/15 , https://ui.adsabs.harvard.edu/abs/2015ApJS..219...15S 219, 15

    2015 doi

  147. [160]

    Shuntov M., et al., 2025, @doi [ ] 10.1051/0004-6361/202452570 , https://ui.adsabs.harvard.edu/abs/2025A&A...695A..20S 695, A20

    2025 doi

  148. [161]

    F., Nelson D., Hernquist L., 2015, @doi [ ] 10.1093/mnras/stv1340 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.452..575S 452, 575

    Sijacki D., Vogelsberger M., Genel S., Springel V., Torrey P., Snyder G. F., Nelson D., Hernquist L., 2015, @doi [ ] 10.1093/mnras/stv1340 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.452..575S 452, 575

    2015 doi

  149. [162]

    Silich S., Tenorio-Tagle G., 2001, @doi [ ] 10.1086/320455 , https://ui.adsabs.harvard.edu/abs/2001ApJ...552...91S 552, 91

    2001 doi

  150. [163]

    Smit R., et al., 2018, @doi [ ] 10.1038/nature24631 , https://ui.adsabs.harvard.edu/abs/2018Natur.553..178S 553, 178

    2018 doi

  151. [164]

    Smith D. J. B., Hayward C. C., 2015, @doi [ ] 10.1093/mnras/stv1727 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.453.1597S 453, 1597

    2015 doi

  152. [165]

    R., Fall S

    Sokolowska A., Capelo P. R., Fall S. M., Mayer L., Shen S., Bonoli S., 2017, @doi [ ] 10.3847/1538-4357/835/2/289 , https://ui.adsabs.harvard.edu/abs/2017ApJ...835..289S 835, 289

    2017 doi

  153. [166]

    S., Gabrielpillai A., Hadzhiyska B., Genel S., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2502.03679 , https://ui.adsabs.harvard.edu/abs/2025arXiv250203679S p

    Somerville R. S., Gabrielpillai A., Hadzhiyska B., Genel S., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2502.03679 , https://ui.adsabs.harvard.edu/abs/2025arXiv250203679S p. arXiv:2502.03679

    2025 doi arXiv

  154. [167]

    Springel V., Hernquist L., 2003, @doi [ ] 10.1046/j.1365-8711.2003.06206.x , https://ui.adsabs.harvard.edu/abs/2003MNRAS.339..289S 339, 289

    2003

  155. [168]

    J., Labb \'e I., Illingworth G

    Stefanon M., Bouwens R. J., Labb \'e I., Illingworth G. D., Gonzalez V., Oesch P. A., 2021, @doi [ ] 10.3847/1538-4357/ac1bb6 , https://ui.adsabs.harvard.edu/abs/2021ApJ...922...29S 922, 29

    2021 doi

  156. [169]

    Stinson G., Seth A., Katz N., Wadsley J., Governato F., Quinn T., 2006, @doi [ ] 10.1111/j.1365-2966.2006.11097.x , https://ui.adsabs.harvard.edu/abs/2006MNRAS.373.1074S 373, 1074

    2006

  157. [170]

    A., Kriek M., Price S

    Suess K. A., Kriek M., Price S. H., Barro G., 2019, @doi [ ] 10.3847/1538-4357/ab1bda , https://ui.adsabs.harvard.edu/abs/2019ApJ...877..103S 877, 103

    2019 doi

  158. [171]

    A., van Albada T

    Swaters R. A., van Albada T. S., van der Hulst J. M., Sancisi R., 2002, @doi [ ] 10.1051/0004-6361:20011755 , https://ui.adsabs.harvard.edu/abs/2002A&A...390..829S 390, 829

    2002 doi

  159. [172]

    G., Trenti M., Illingworth G

    Szomoru D., Franx M., van Dokkum P. G., Trenti M., Illingworth G. D., Labb \'e I., Oesch P., 2013, @doi [ ] 10.1088/0004-637X/763/2/73 , https://ui.adsabs.harvard.edu/abs/2013ApJ...763...73S 763, 73

    2013 doi

  160. [173]

    J., Genzel R., Sternberg A., 2020, @doi [ ] 10.1146/annurev-astro-082812-141034 , https://ui.adsabs.harvard.edu/abs/2020ARA&A..58..157T 58, 157

    Tacconi L. J., Genzel R., Sternberg A., 2020, @doi [ ] 10.1146/annurev-astro-082812-141034 , https://ui.adsabs.harvard.edu/abs/2020ARA&A..58..157T 58, 157

    2020 doi

  161. [174]

    R., Babul A., Madau P., Capelo P

    Tamfal T., Mayer L., Quinn T. R., Babul A., Madau P., Capelo P. R., Shen S., Staub M., 2022, @doi [ ] 10.3847/1538-4357/ac558e , https://ui.adsabs.harvard.edu/abs/2022ApJ...928..106T 928, 106

    2022 doi

  162. [175]

    K., Nomoto K., Yokoi K., 1986, , https://ui.adsabs.harvard.edu/abs/1986A&A...158...17T 158, 17

    Thielemann F. K., Nomoto K., Yokoi K., 1986, , https://ui.adsabs.harvard.edu/abs/1986A&A...158...17T 158, 17

    1986

  163. [176]

    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

  164. [177]

    R., Pontzen A., Anderson L., Bellovary J., 2017, @doi [ ] 10.1093/mnras/stx1160 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.470.1121T 470, 1121

    Tremmel M., Karcher M., Governato F., Volonteri M., Quinn T. R., Pontzen A., Anderson L., Bellovary J., 2017, @doi [ ] 10.1093/mnras/stx1160 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.470.1121T 470, 1121

    2017 doi

  165. [178]

    Tremmel M., et al., 2019, @doi [ ] 10.1093/mnras/sty3336 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.483.3336T 483, 3336

    2019 doi

  166. [179]

    Trinca A., Schneider R., Valiante R., Graziani L., Ferrotti A., Omukai K., Chon S., 2024, @doi [ ] 10.1093/mnras/stae651 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.529.3563T 529, 3563

    2024 doi

  167. [180]

    J., Bundy K., Cooper M

    Trujillo I., Conselice C. J., Bundy K., Cooper M. C., Eisenhardt P., Ellis R. S., 2007, @doi [ ] 10.1111/j.1365-2966.2007.12388.x , https://ui.adsabs.harvard.edu/abs/2007MNRAS.382..109T 382, 109

    2007

  168. [181]

    Vega-Ferrero J., et al., 2024, @doi [ ] 10.3847/1538-4357/ad05bb , https://ui.adsabs.harvard.edu/abs/2024ApJ...961...51V 961, 51

    2024 doi

  169. [182]

    Walter F., Brinks E., de Blok W. J. G., Bigiel F., Kennicutt Jr. R. C., Thornley M. D., Leroy A., 2008, @doi [ ] 10.1088/0004-6256/136/6/2563 , https://ui.adsabs.harvard.edu/abs/2008AJ....136.2563W 136, 2563

    2008 doi

  170. [183]

    Wang J., et al., 2013, @doi [ ] 10.1093/mnras/stt722 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.433..270W 433, 270

    2013 doi

  171. [184]

    Wang J., Catinella B., Saintonge A., Pan Z., Serra P., Shao L., 2020, @doi [ ] 10.3847/1538-4357/ab68dd , https://ui.adsabs.harvard.edu/abs/2020ApJ...890...63W 890, 63

    2020 doi

  172. [185]

    Ward E., et al., 2024, @doi [ ] 10.3847/1538-4357/ad20ed , https://ui.adsabs.harvard.edu/abs/2024ApJ...962..176W 962, 176

    2024 doi

  173. [186]

    Weidemann V., 1987, , https://ui.adsabs.harvard.edu/abs/1987A&A...188...74W 188, 74

    1987

  174. [187]

    in Comput

    Wendland H., 1995, @doi [Adv. in Comput. Math.] 10.1007/BF02123482 , 4, 389

    1995 doi

  175. [188]

    M., Feng Y., Di-Matteo T., Croft R., Stanway E

    Wilkins S. M., Feng Y., Di-Matteo T., Croft R., Stanway E. R., Bunker A., Waters D., Lovell C., 2016, @doi [ ] 10.1093/mnras/stw1154 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.460.3170W 460, 3170

    2016 doi

  176. [189]

    M., Feng Y., Di Matteo T., Croft R., Lovell C

    Wilkins S. M., Feng Y., Di Matteo T., Croft R., Lovell C. C., Waters D., 2017, @doi [ ] 10.1093/mnras/stx841 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.469.2517W 469, 2517

    2017 doi

  177. [190]

    H., Norman M

    Xu H., Wise J. H., Norman M. L., Ahn K., O'Shea B. W., 2016, @doi [ ] 10.3847/1538-4357/833/1/84 , https://ui.adsabs.harvard.edu/abs/2016ApJ...833...84X 833, 84

    2016 doi

  178. [191]

    Xu Y., et al., 2024, @doi [ ] 10.3847/1538-4357/ad82dd , https://ui.adsabs.harvard.edu/abs/2024ApJ...976..142X 976, 142

    2024 doi

  179. [192]

    Yajima H., Abe M., Fukushima H., Ono Y., Harikane Y., Ouchi M., Hashimoto T., Khochfar S., 2023, @doi [ ] 10.1093/mnras/stad2497 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.525.4832Y 525, 4832

    2023 doi

  180. [193]

    arXiv:2504.07185

    Yang L., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2504.07185 , https://ui.adsabs.harvard.edu/abs/2025arXiv250407185Y p. arXiv:2504.07185

    2025 doi arXiv

  181. [194]

    Yeh J. Y. C., et al., 2023, @doi [ ] 10.1093/mnras/stad210 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.520.2757Y 520, 2757

    2023 doi

  182. [195]

    Yung L. Y. A., Somerville R. S., Finkelstein S. L., Wilkins S. M., Gardner J. P., 2024, @doi [ ] 10.1093/mnras/stad3484 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.527.5929Y 527, 5929

    2024 doi

  183. [196]

    G., et al., 2008, @doi [ ] 10.1086/587874 , https://ui.adsabs.harvard.edu/abs/2008ApJ...677L...5V 677, L5

    van Dokkum P. G., et al., 2008, @doi [ ] 10.1086/587874 , https://ui.adsabs.harvard.edu/abs/2008ApJ...677L...5V 677, L5

    2008 doi

  184. [197]

    G., et al., 2010, @doi [ ] 10.1088/0004-637X/709/2/1018 , https://ui.adsabs.harvard.edu/abs/2010ApJ...709.1018V 709, 1018

    van Dokkum P. G., et al., 2010, @doi [ ] 10.1088/0004-637X/709/2/1018 , https://ui.adsabs.harvard.edu/abs/2010ApJ...709.1018V 709, 1018

    2010 doi

  185. [198]

    van Donkelaar F., Agertz O., Renaud F., 2022, @doi [ ] 10.1093/mnras/stac692 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.512.3806V 512, 3806

    2022 doi

  186. [199]

    R., Tamfal T., Quinn T

    van Donkelaar F., Mayer L., Capelo P. R., Tamfal T., Quinn T. R., Madau P., 2023, @doi [ ] 10.1093/mnras/stad946 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.522.1726V 522, 1726

    2023 doi

  187. [200]

    R., Madau P., 2025, @doi [ ] 10.1093/mnras/staf597 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.539.1259V 539, 1259

    van Donkelaar F., Mayer L., Capelo P. R., Madau P., 2025, @doi [ ] 10.1093/mnras/staf597 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.539.1259V 539, 1259

    2025 doi

  188. [201]

    van der Wel A., et al., 2014, @doi [ ] 10.1088/0004-637X/788/1/28 , https://ui.adsabs.harvard.edu/abs/2014ApJ...788...28V 788, 28

    2014 doi

Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.