Pith. sign in

REVIEW 4 major objections 4 minor 199 references

The paper claims that JWST's 'impossible' early galaxies become ordinary once the observed redshift is split between cosmic expansion and tired light.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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

T0 review · deepseek-v4-flash

2026-08-04 10:18 UTC pith:XEKXVJQE

load-bearing objection Application of CCC+TL to JWST size/mass/density tensions—new transfer functions and worked examples, but the size effect rests on a tired-light component partly fitted to the same data and the luminosity derivation has a fixable algebra error. the 4 major comments →

arxiv 2510.13844 v1 pith:XEKXVJQE submitted 2025-10-11 physics.gen-ph

Evolution of Size, Mass, and Density of Galaxies Since Cosmic Dawn

Rajendra P. Gupta This is my paper
classification physics.gen-ph
keywords galaxy evolutionhigh-redshift galaxiesearly universetired lightcovarying coupling constantsangular diameter distanceJWST early galaxiesgalaxy size-mass-density relation
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper argues that the JWST-era puzzle—galaxies at cosmic dawn that look too massive, too compact, too dense, and too early to have formed—is an artifact of assuming all redshift comes from cosmic expansion. Reinterpreting the same observations in a cosmology where fundamental constants co-vary and a tired-light component shares the redshift, the angular-diameter distance grows much faster with redshift. As a result, inferred galaxy radii increase as (1+z)^0.93, dynamical masses scale up, number densities fall by up to (1+z)^-2.80, and the early universe is about ten times older near z=10. The paper concludes that early galaxies and little red dots no longer require exotic formation channels such as super-Eddington black hole growth.

Core claim

The central claim is that the observed redshift z should be factored as (1+z)=(1+z_x)(1+z_t), with z_x from expansion and z_t from tired light, and that the angular-diameter distance in this CTL model, d_A = f(z_x)d_p(z_x)/(1+z), rises far more steeply than in ΛCDM. Because an object's physical size is d_A times its observed angular size, all galaxies and little red dots become larger as redshift increases—by a factor of about (1+z)^0.93 compared with ΛCDM estimates. The same enlargement raises dynamical masses, lowers surface/volume/number densities, and, together with the model's slower aging, stretches the time available for galaxy assembly. The paper presents ratios of size, luminosity,

What carries the argument

The carrying mechanism is the CTL angular-diameter distance relation d_A(z) = f(z_x)d_p(z_x)/(1+z), built from the redshift split (1+z)=(1+z_x)(1+z_t). Equating the proper distance traveled by a photon under the two redshift causes fixes the split without extra free parameters, and the extra f(z_x) factor makes d_A grow much faster than the ΛCDM angular-diameter distance at z>1. That single ratio drives all the paper's derived corrections: size scales as (d_Ax/d_AΛ), luminosity scales as d_A^2 with additional redshift factors, dynamical mass scales with size, and densities scale as inverse powers of size.

Load-bearing premise

The load-bearing premise is that tired light is real and contributes to the observed redshift, splitting it cleanly into an expansion part and a tired-light part; the paper states the mechanism is currently unknown, and the model was introduced partly because CCC alone failed the JWST size data.

What would settle it

A decisive test is the distance-duality relation: measure luminosity distances from standard candles and angular-diameter distances from independent geometric probes at z≈1–3 and beyond. CTL predicts a specific deviation because time dilation and photon energy loss apply only partly to the expansion redshift; if the standard relation d_L=(1+z)^2 d_A holds, the tired-light split—and with it the (1+z)^0.93 size enlargement—is falsified.

Watch this falsifier. Get emailed when new claim-graph text bears on it.

If this is right

  • The JWST galaxy JADES-GS-z14-0, with a ΛCDM UV radius of about 260 pc at z=14.18, would have a radius of about 3.2 kpc in the CTL model; compact early galaxies are not inherently compact.
  • Dynamical masses of high-redshift galaxies are substantially higher while stellar masses rise only modestly (factor ~1.7 at z=14), so the stellar-to-dynamical mass ratio drops for that galaxy from ~2 to ~1/14, consistent with gas-dominated young systems.
  • Number densities of quiescent and ultra-massive galaxies drop by factors of hundreds at z~5–7, aligning observed abundances with model predictions rather than exceeding them by 100–1000 times.
  • At z=10 the model gives the universe roughly ten times more time than ΛCDM; a 280 Myr-old universe at z=15 becomes 4.35 Gyr, removing the need for unrealistically rapid star formation and super-Eddington black hole accretion.
  • Luminosity and stellar-mass corrections are small (a factor up to ~1.8 at z=20), so the model identifies size, not brightness, as the main resolution of the early-galaxy tension.

Where Pith is reading between the lines

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

  • The same redshift split implies a testable violation of the standard distance-duality relation d_L=(1+z)^2 d_A; a high-redshift measurement comparing standard-candle distances with geometric or angular-diameter distances could confirm or kill the tired-light component.
  • The (1+z)^0.93 correction is universal in this model, so it can be applied to published size-mass evolution slopes: any survey fitted with r_e ∝ (1+z)^s should show s+0.93 if CTL is right, a prediction existing JWST catalogs can check immediately.
  • If the model's enlarged radii are correct, gas fractions and star formation efficiencies inferred from dynamical-to-stellar mass ratios at z>5 will be much higher than currently reported, shifting interpretations of early metal enrichment.
  • Because the tired-light mechanism is unspecified, the size correction is currently a phenomenological rescaling; a physical derivation of the TL component would turn these ratios into quantitative predictions about photon interactions over cosmological distances.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

4 major / 4 minor

Summary. The paper argues that the CCC+TL cosmology—an alternative to ΛCDM with covarying coupling constants and a tired-light component—predicts larger angular-diameter distances at high redshift, and hence larger physical sizes, lower inferred densities, and modestly higher luminosities for galaxies observed by JWST. It derives ratios for size, luminosity/mass, and density relative to ΛCDM, fits the size ratio as r_e ∝ (1+z)^0.93, and applies the scalings to specific objects (JADES-GS-z14-0, Abell2744-QSO1, Little Red Dots, RUBIES-UDS-QG-z7). It concludes that the early-galaxy tensions in ΛCDM are largely resolved in CTL.

Significance. If the CTL model is taken as given, the size-enlargement result follows directly from the ratio d_A^CTL/d_A^Λ and is a useful consistency check for the model. The paper is clearly organized and compiles many current JWST results, making concrete quantitative predictions that can in principle be checked. However, its quantitative claims for luminosity, stellar mass, and number density are compromised by an algebraic error and missing model parameters, and the central size effect relies on the tired-light split that was introduced specifically to address JWST galaxy sizes, making the 'prediction' partly circular. The paper's strengths—clear structure, specific applications, and acknowledgment of the unknown TL mechanism—do not outweigh these issues.

major comments (4)
  1. [Section 3, Eqs. (12) and (14)] The derivation chain for the luminosity ratio is internally inconsistent. Equating fluxes before Eq. (12) gives L_Λ/d_pΛ^2 = L_x (1+z_t)/d_px^2, which implies L_x = L_Λ (d_px^2/d_pΛ^2)/(1+z_t); the printed Eq. (12) has (1+z_t) in the numerator. Equation (14), used for Figure 3 and Table 1, matches the corrected denominator version (with (1+z_t)^3). Thus a reader following the printed equations cannot reproduce the luminosity ratios, and the figures/table rely on an unstated correction. Please fix Eq. (12) and re-verify all quoted luminosity and stellar-mass ratios, including the abstract's luminosity factor 1.8 at z=20.
  2. [Section 2, Eqs. (8)–(11) and Figure 1] The CTL angular-diameter distance—and therefore the central r_e ∝ (1+z)^0.93 result, the density scalings, and every entry in Table 1—depends on the model parameters α, H0, and the resulting z_x(z) and f(z_x) split. None of these are given in this paper. Without them, the curves in Figures 1–5, the exponent 0.93, and the numerical factors in Table 1 cannot be independently checked. Please provide the fitted parameter values, a formula or table for z_x(z), and the numerical form of f(z_x), or a clear pointer to a publicly available implementation.
  3. [Section 2, paragraph after Eq. (11); Section 4] The tired-light component is load-bearing for the size enlargement—without it the (1+z)^0.93 correction disappears—but the text states that TL was invoked in ref. [86] only after CCC alone was 'unsatisfactory in explaining the JWST galaxy size data at cosmic dawn,' and that the TL mechanism is 'currently unknown.' The agreement with JWST sizes is therefore partly an accommodation of the target data rather than an independent prediction. Please clearly separate 'accommodated' from 'predicted' and suggest out-of-sample tests (e.g., CMB spectral distortions, redshift drift, or surface-brightness tests) that do not use the data that motivated the TL admixture.
  4. [Section 3 'Density Decrease' and abstract 'number density by (1+z)^{-2.80}'] The paper applies the object-volume scaling d_A^{-3} to the number density of galaxies in surveys (e.g., the factor ~385 at z=7 for RUBIES-UDS-QG-z7, and the abstract's exponent -2.80). For survey number densities, the relevant volume element is the comoving volume element, which scales as D_M^2 (dχ/dz), not simply as d_A^3. The two are equal only under additional assumptions about how the line-of-sight distance changes. Please derive the number-density modification from the CTL metric volume element and state whether the quoted factors are physical-volume or comoving-volume densities.
minor comments (4)
  1. [Section 4] The phrase 'the question becomes mute' should read 'the question becomes moot.'
  2. [Figures 1–5] The figures give no indication of the parameter values, the numerical integration used, or uncertainties. Adding a short caption note or appendix with the parameter values would greatly improve reproducibility.
  3. [Section 4, Table 1] The table ignores uncertainties, which is acceptable for illustration, but the caption should state this explicitly. Also, the 'Number den. LRD' row appears to be a placeholder rather than a computed value; please clarify.
  4. [References] There are a few typographical issues in the reference list (e.g., ref. 113, 'misión' for 'mission'). A careful proofread is recommended.

Circularity Check

2 steps flagged

The claimed r_e∝(1+z)^{0.93} correction is a restatement of the tired-light ansatz introduced in ref. [86] to fit the same JWST size data it is used to reinterpret.

specific steps
  1. ansatz smuggled in via citation [Section 2, paragraph following Eq. (11); also TL limitations paragraph]
    "It was shown in an earlier paper [86] that while the CCC and the ΛCDM models are great in fitting the low redshift observations, e.g., Pantheon+ supernova type Ia data, both of them are unsatisfactory in explaining the JWST galaxy size data at cosmic dawn and reionization redshifts. We then invoked the tired-light (TL) concept of Zwicky [85] to coexist in the expanding Universe."

    The size enlargement used throughout the paper is the CTL/ΛCDM angular-diameter-distance ratio, with d_Ax = d_px f(z_x)/(1+z_x) and (1+z)=(1+z_x)(1+z_t) (Eqs. 11-13). The TL split is the ingredient that makes d_Ax grow faster than d_AΛ; the paper acknowledges CCC alone was unsatisfactory for JWST sizes and that TL's mechanism is 'currently unknown.' Thus the TL component was adopted in ref. [86] to accommodate the same JWST angular-size data whose tension this paper reinterprets as a predicted r_e∝(1+z)^{0.93} correction. The central result is therefore a restatement, via self-citation, of an ansatz chosen to fit the target phenomenon rather than an independent first-principles prediction.

  2. self definitional [Section 4, 'Size Evolution' paragraph; Section 3, 'Size Increase']
    "We also show the inverse of the power-law fit, 𝑅𝑒 = (1 + 𝑧)0.93, for the increase in the physical size of the objects in the CTL (labeled as CCC+TL) model compared to the ΛCDM model."

    Section 3 defines the size increase as 'taking the ratio of d_A in the CTL and ΛCDM models,' and physical size is proportional to d_A by definition. The quoted 0.93 exponent is described as the inverse of a power-law fit to that model-generated ratio curve. Consequently r_e∝(1+z)^{s+0.93} is a summary of the definitional d_A ratio, not a parameter-free observable prediction. Combined with the TL ansatz imported from [86], the corrected size evolution is forced by the model input rather than tested against it.

full rationale

The paper's corrections are computed from the ratio of the CTL and ΛCDM angular-diameter distances; this is an algebraic consequence of Eqs. (11)-(13), not an independently measured or simulated result. The paper explicitly states that the tired-light component was introduced in prior work [86] only after CCC and ΛCDM both failed to explain the JWST galaxy size data, and that the TL mechanism is 'currently unknown.' Since that TL split is exactly what makes d_Ax/d_AΛ grow with z, the headline 'size increase' r_e∝(1+z)^{0.93} restates the model choice made to fit the target data; the exponent is a fit to the model's own ratio curve. The consistency claims (Pantheon+, BAO, CMB, etc.) are carried by self-citations [86-89] rather than demonstrated in this paper. Separately, the printed luminosity derivation is internally inconsistent: Eq. (12) places (1+z_t) in the numerator while Eq. (14) requires it in the denominator, so the luminosity/mass corrections cannot be reproduced from the paper's equations as written; this is a correctness problem, not counted as circularity. On the circularity axis, the central claim reduces to an ansatz adopted to fix the same anomaly it is used to explain, giving score 7.

Axiom & Free-Parameter Ledger

2 free parameters · 6 axioms · 2 invented entities

The rescaling calculation depends almost entirely on the prior CCC+TL model: the exponential form of f(t), the TL redshift split, and the modified Friedmann equations. The free parameter α is fitted to Pantheon+ data in earlier papers and is not given here. No new entity has independent evidence outside the model itself.

free parameters (2)
  • α (CCC coupling evolution constant) = not stated in this paper
    Defines f(t)=exp(α(t−t0)); enters H(z), proper distance, and hence all angular-diameter-distance rescaling exponents.
  • H0 (Hubble constant in CTL) = not stated in this paper
    Together with α sets the angular-diameter-distance scale; obtained from the Pantheon+ fit in previous works by the same author.
axioms (6)
  • domain assumption Coupling constants covary as c∝f(t), G∝f(t)^3, ℏ∝f(t)^2, kB∝f(t)^2.
    Adopted from ref [84] (same author); no derivation in this paper; underlies the modified Friedmann equations (Eqs 2–4).
  • ad hoc to paper f(t)=exp(α(t−t0)) with α an unknown constant.
    Chosen 'to be consistent with Occam's razor'; not derived; central to H(z), d_p, and d_A.
  • domain assumption Tired light contributes to the observed redshift alongside expansion, with (1+z)=(1+z_x)(1+z_t), and the proper distance traversed is the same for both effects.
    Invoked in Section 2 following Eq (11); mechanism unknown and acknowledged in the text; drives the d_A enhancement that produces the size correction.
  • domain assumption Flat, matter-dominated universe with Ωr≪Ωm and no dark energy.
    Used to simplify Eq (7) to Eq (8); not central to the ratio comparison but assumed throughout.
  • domain assumption Mass-to-light ratio Y* ≡ M*/L is constant.
    Explicitly assumed in Section 3 before 'Mass Increase'; if false, the stellar-mass rescaling is not simply L_x/L_Λ.
  • domain assumption Modified Einstein equations from Costa et al. and the author's prior papers are valid and general covariance can be maintained.
    Section 2 addresses covariance by citing refs [129–132] but does not demonstrate it in this paper.
invented entities (2)
  • Tired-light photon-energy-loss mechanism no independent evidence
    purpose: Produces the TL redshift component z_t and yields the d_Ax growth relative to ΛCDM, which is the basis for the size/mass/density corrections.
    The paper states 'It is currently unknown and the subject of ongoing research'; no independent falsifiable handle is presented.
  • Covarying coupling function f(t) with G∝f^3, c∝f, etc. no independent evidence
    purpose: Modifies the FLRW metric and Friedmann equations, stretching distances and ages.
    No direct measurement of a varying G or c is provided; the paper argues existing constraints are invalid because other constants were held fixed.

pith-pipeline@v1.3.0-alltime-deepseek · 28619 in / 18710 out tokens · 161018 ms · 2026-08-04T10:18:39.138958+00:00 · methodology

0 comments
read the original abstract

The formation and evolution of galaxies and other astrophysical objects have become of great interest, especially since the launch of the James Webb Space Telescope in 2021. The mass, size, and density of objects in the early universe appear to be drastically different from those predicted by the standard cosmology - the $\Lambda$CDM model. This work shows that the mass-size-density evolution is not surprising when we use the CCC+TL cosmology, which is based on the concepts of covarying coupling constants in an expanding universe and the tired light effect contributing to the observed redshift. This model is consistent with supernovae Pantheon+ data, the angular size of the cosmic dawn galaxies, BAO, CMB sound horizon, galaxy formation time scales, time dilation, galaxy rotation curves, etc., and does not have the coincidence problem. The effective radii $r_e$ of the objects are larger in the new model by $r_e \propto (1+z)^{0.93}$. Thus, the object size evolution in different studies, estimated as $r_e \propto (1+z)^s$ with $s=-1.0 \pm {0.3}$, is modified to $r_e \propto (1+z)^{s+0.93}$, the dynamical mass by $(1+z)^{0.93}$, and number density by $(1+z)^{-2.80}$. The luminosity modification increases slowly with $z$ to 1.8 at $z=20$. Thus, the stellar mass increase is modest, and the luminosity and stellar density decrease are mainly due to the larger object size in the new model. Since the aging of the universe is stretched in the new model, its temporal evolution is much slower (e.g., at $z=10$, the age is about a dex longer); stars, black holes, and galaxies do not have to form at unrealistic rates.

Figures

Figures reproduced from arXiv: 2510.13844 by Rajendra P. Gupta.

Figure 1
Figure 1. Figure 1: presents the angular diameter distance 𝑑𝐴 for the two models based on the model parameters obtained by fitting Pantheon+ data. We notice that except for low redshifts, 𝑑𝐴 is vastly different for the two models. And, since the physical size of an object of a measured angular size is directly proportional to 𝑑𝐴, it is also very different in the two models [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: The age comparison for the CTL and the ΛCDM models as age ratio at different redshifts 𝑧. The abscissa shows the redshift 𝑧 as well as the corresponding age of the Universe in the two models for ready reference. 3. Results Our focus in this paper is on the CTL model and comparing the results with its ΛCDM equivalent. The CTL model offers a fundamentally different cosmological per￾spective compared to the Λ… view at source ↗
Figure 3
Figure 3. Figure 3: Comparison of the stellar mass M*, Luminosity, dynamical mass 𝑀dyn, and size R for the CTL and the ΛCDM models in the form of their ratios at different redshifts 𝑧. The abscissa shows the redshift 𝑧 as well as the corresponding age of the Universe in the two models for ready reference. Black hole mass is considered proportional to the luminosity of 𝐻𝛼 (𝐻𝛽) lines: 𝑀𝐵𝐻 ∝ 𝐿 0.55(0.56) [143-144]. Thus, black h… view at source ↗
Figure 4
Figure 4. Figure 4: Comparison of the dynamical mass 𝑀dyn and stellar mass M* evolution in the CTL model relative to the ΛCDM models in the form of their ratios at different redshifts 𝑧. The abscis- [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of the evolution of some densities in the CTL model relative to the ΛCDM models in the form of their ratios at different redshifts 𝑧. The abscissa shows the redshift 𝑧 as well as the corresponding age of the Universe in the two models for ready reference. 4. Discussion Having compared the size-mass-density evolution with the redshift in the two models, we need to see how the results of the previ… view at source ↗
Figure 6
Figure 6. Figure 6: Comparison of the evolution of the effective radius 𝑅𝑒 of galaxies with redshift 𝑧 in different studies shown in the legend [77-80, 150] and discussed in the text. Mass Evolution: As discussed above, while stellar and black hole masses depend on luminosities, the dynamical mass, i.e., total mass, is related to the effective radius and dispersion velocity. Many high-redshift galaxies appear to have stellar-… view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

199 extracted references · 1 canonical work pages

  1. [1]

    Two Remarkably Luminous Galaxy Candidates at z ≈ 10–12 Revealed by JWST

    Naidu, R.P.; Oesch, P.A.; van Dokkum, P.; Nelson, E.J.; Suess, K.A.; Brammer, G.; Whitaker, K.E.; Illingworth, G.; Bouwens, R.; Tacchella, S. Two Remarkably Luminous Galaxy Candidates at z ≈ 10–12 Revealed by JWST. Astrophys. J. Lett. 2022, 940, L14

    2022

  2. [2]

    Schrodinger’s Galaxy Candidate: Puzzlingly Luminous at z ≈ 17, or Dusty/Quenched at z ≈ 5? arXiv 2022, arXiv:2208.02794

    Naidu, R.P.; Oesch, P.A.; Setton, D.J.; Matthee, J.; Conroy, C.; Johnson, B.D.; Weaver, J.R.; Bouwens, R.J.; Brammer, G.B.; Dayal, P.; et al . Schrodinger’s Galaxy Candidate: Puzzlingly Luminous at z ≈ 17, or Dusty/Quenched at z ≈ 5? arXiv 2022, arXiv:2208.02794

    Pith/arXiv arXiv 2022

  3. [3]

    A population of red candidate massive galaxies ~600 Myr after the Big Bang

    Labbé, I.; van Dokkum, P.; Nelson, E.; Bezanson, R.; Suess, K.A.; Leja, J.; Brammer, G.; Whitaker, K.; Mathews, E.; Stefanon, M.; et al. A population of red candidate massive galaxies ~600 Myr after the Big Bang. Nature 2023, 616, 266

    2023

  4. [4]

    Spectroscopic confirmation of four metal-poor galaxies at z = 10.3–13.2

    Curtis-Lake, E.; Carniani, S.; Cameron, A.; Charlot, S.; Jakobsen, P.; Maiolino, R.; Bunker, A.; Witstok, J.; Smit, R.; Chevallard, J.; et al. Spectroscopic confirmation of four metal-poor galaxies at z = 10.3–13.2. Nat. Astron. 2023, 7, 622

    2023

  5. [5]

    UNCO- VER: Illuminating the Early Universe—JWST/NIRSpec Confirmation of z > 12 Galaxies

    Wang, B.; Fujimoto, S.; Labbé, I.; Furtak, L.J.; Miller, T.B.; Setton, D.J.; Zitrin, A.; Atek, H.; Bezanson, R.; Brammer , G. UNCO- VER: Illuminating the Early Universe—JWST/NIRSpec Confirmation of z > 12 Galaxies. Astrophys. J. Lett. 2023, 957, L34

    2023

  6. [6]

    Searching for Emission Lines at z > 11: The Role of Damped L yman-α and Hints About the Escape of Ionizing Photons

    Hainline, K.N.; D ’Eugenio, F.; Jakobsen, P.; Chevallard, J.; Carniani, S.; Witstok, J.; Ji, Z.; Curtis -Lake, E.; Johnson, B.D.; Ro b- ertson, B.; et al. Searching for Emission Lines at z > 11: The Role of Damped L yman-α and Hints About the Escape of Ionizing Photons. arXiv 2024, arXiv: 2404.04325

    Pith/arXiv arXiv 2024

  7. [7]

    Spectroscopic confirmation of two luminous galaxies at a redshift of 14

    Carniani, S.; Hainline, K.; D’Eugenio, F.; Eisenstein, D.J.; Jakobsen, P.; Witstok, J.; Johnson, B.D.; Chevallard, J.; Maioli no, R.; Helton, J.M.; et al. Spectroscopic confirmation of two luminous galaxies at a redshift of 14. Nature 2024, 633, 318

    2024

  8. [8]

    Accelerated formation of ultra-massive galaxies in the first billion years

    Xiao, M.; Oesch, P.A.; Elbaz, D.; Bing, L.; Nelson, E.J.; Weibel, A.; Illingworth, G.D.; van Dokkum, P.; Naidu, R.P.; Daddi, E.; et al. Accelerated formation of ultra-massive galaxies in the first billion years. Nature 2024, 635, 311

    2024

  9. [9]

    Unveiling the hidden Universe with JWST: The con tribution of dust-obscured galaxies to the stellar mass function at z ~ 3–8

    Gottumukkala, R.; Barrufet, L.; Oesch, P.A.; Weibel, A.; Allen, N.; Pampliega, B.A.; Nelson, E.J.; Williams, C.C.; Brammer, G .; Fudamoto, Y.; et al. Unveiling the hidden Universe with JWST: The con tribution of dust-obscured galaxies to the stellar mass function at z ~ 3–8. Mon. Not. R. Astron. Soc. 2024, 530, 966. https://doi.org/10.1093/mnras/stae754

    doi:10.1093/mnras/stae754 2024

  10. [10]

    RUBIES Reveals a Massive Quiescent Galaxy at z = 7.3

    Weibel, A.; de Graaff, A.; Setton, D.J.; Miller, T.B.; Oesch, P.A.; Brammer, G.; Lagos, C.D.P.; Whitaker, K.E.; Williams, C.C.; Baggen, J.F.W.; et al. RUBIES Reveals a Massive Quiescent Galaxy at z = 7.3. Astrophys. J. 2025, 983, 11

    2025

  11. [11]

    A Comprehensive Study of Galaxies at z ~ 9–16 Found in the Early JWST Data: Ultraviolet Luminosity Functions and Cosmic Star Formation History at the Pre-reionization Epoch

    Harikane, Y.; Ouchi, M.; Oguri, M.; Ono, Y.; Nakajima, K.; Isobe, Y.; Umeda, H.; Mawatari, K.; Zhang, Y. A Comprehensive Study of Galaxies at z ~ 9–16 Found in the Early JWST Data: Ultraviolet Luminosity Functions and Cosmic Star Formation History at the Pre-reionization Epoch. Astrophys. J. Suppl. Ser. 2023, 265, 5

    2023

  12. [12]

    The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ~ 8.5–14.5

    Finkelstein, S.L.; Leung, G.C.K.; Bagley, M.B.; Dickinson, M.; Ferguson, H.C.; Papovich, C.; Akins, H.B.; Haro, P.A.; Davé, R.; Dekel, A.; et al . The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ~ 8.5–14.5. Astrophys. J. Lett. 2024, 969, L2. 15 of 22

    2024

  13. [13]

    COSMOS-Web: Intrinsically Luminous z ≳ 10 Galaxy Candidates Test Early Stellar Mass Assembly

    Casey, C.M.; Akins, H.B.; Shuntov, M.; Ilbert, O.; Paquereau, L.; Franco, M.; Hayward, C.C.; Finkelstein, S.L.; Boylan -Kolchin, M.; Robertson, B.E.; et al. COSMOS-Web: Intrinsically Luminous z ≳ 10 Galaxy Candidates Test Early Stellar Mass Assembly. Astrophys. J. 2024, 965, 98

    2024

  14. [14]

    Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosm ic Star Formation Rate Densi- ty 300 Myr after the Big Bang

    Robertson, B.E.; Johnson, B.D.; Tacchella, S.; Eisenstein, D.J.; Hainline, K.; Arribas, S.; Baker, W.M.; Bunker, A.J.; Carniani, S.; Cargile, P.A.; et al. Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosm ic Star Formation Rate Densi- ty 300 Myr after the Big Bang. Astrophys. J. 2024, 970, 31

    2024

  15. [15]

    JWST PRIMER: A new mu lti-field determination of the evolving galaxy UV luminosity function at re d- shifts z ≃ 9–15

    Donnan, C.T.; McLure, R.J.; Dunlop, J.S.; McLeod, D.J.; Magee, D.; Arellano-Córdova, K.Z.; Barrufet, L.; Begley, R.; Bowler, R.A.A.; Carnall, A.C. JWST PRIMER: A new mu lti-field determination of the evolving galaxy UV luminosity function at re d- shifts z ≃ 9–15. arXiv 2024, arXiv: 2403.03171

    Pith/arXiv arXiv 2024

  16. [16]

    Discovery and properties of ultra -high redshift galaxies (9 < z < 12) in the JWST ERO SMACS 0723 Field

    Adams, N.J.; Conselice, C.J.; Ferreira, L.; Austin, D.; Trussler, J.; Juodžbalis, I.; Wilkins, S.M.; Caruana, J.; Dayal, P.; Verma, A.; et al. Discovery and properties of ultra -high redshift galaxies (9 < z < 12) in the JWST ERO SMACS 0723 Field . Mon. Not. R. Astron. Soc. 2023, 518, 4755. https://doi.org/10.1093/mnras/stac3347

    doi:10.1093/mnras/stac3347 2023

  17. [17]

    Revealing Galaxy Candidates out to z ~ 16 with JWST Observations of the Lensing Cluster SMACS0723

    Atek, H.; Shuntov, M.; Furtak, L.J.; Richard, J.; Kneib, J.-P.; Mahler, G.; Zitrin, A.; McCracken, H.J.; Charlot, S.; Chevallard, J. Revealing Galaxy Candidates out to z ~ 16 with JWST Observations of the Lensing Cluster SMACS0723 . arXiv 2022, arXiv:2207.12338

    Pith/arXiv arXiv 2022

  18. [18]

    JWST/NIRCam observations of stars and H ii regions in z ≃ 6–8 galaxies: Properties of star-forming complexes on 150 pc scales

    Chen, Z.; Stark, D.P.; Endsley, R.; Topping, M.; Whi tler, L.; Charlot, S. JWST/NIRCam observations of stars and H ii regions in z ≃ 6–8 galaxies: Properties of star-forming complexes on 150 pc scales. arXiv 2022, arXiv:2207.12657

    Pith/arXiv arXiv 2022

  19. [19]

    Begley, R.; Cullen, F.; Hamadouche, M.L.; Bowler, R.A.A.; Magee, D

    Donnan, C.T.; McLeod, D.J.; Dunlop, J.S.; McLure, R.J.; Carnall, A.C. ; Begley, R.; Cullen, F.; Hamadouche, M.L.; Bowler, R.A.A.; Magee, D. The evolution of the galaxy UV luminosity function at redshifts z ≃ 8–15 from deep JWST and ground-based near-infrared imaging. Mon. Not. R. Astron. Soc. 2023, 518, 6011. https://doi.org/10.1093/mnras/stac3472

    doi:10.1093/mnras/stac3472 2023

  20. [20]

    A Long Time Ago in a Galaxy Far, Far Away: A Candidate z ~ 12 Galaxy in Early JWST CEERS Imaging

    Finkelstein, S.L.; Bagley, M.B.; Haro, P.A.; Dickinson, M.; Ferguson, H.C.; Kartaltepe, J.S.; Papovich, C.; Burgarella, D.; Koce- vski, D.D.; Huertas-Company, M.; et al . A Long Time Ago in a Galaxy Far, Far Away: A Candidate z ~ 12 Galaxy in Early JWST CEERS Imaging. Astrophys. J. Lett. 2022, 940, L55

    2022

  21. [21]

    Morphologies of Galaxies at z ≳ 9 Uncovered by JWST/NIRCam Imaging: Cosmic Size Evolution and an Identification of an Extremely Compact Bright Galaxy at z ~ 12

    Ono, Y.; Harikane, Y.; Ouchi, M.; Yajima, H.; Abe, M.; Isobe, Y.; Shibuya, T.; Wise, J.H.; Zhang, Y.; Nakajima, K.; et al. Morphologies of Galaxies at z ≳ 9 Uncovered by JWST/NIRCam Imaging: Cosmic Size Evolution and an Identification of an Extremely Compact Bright Galaxy at z ~ 12. Astrophys. J. 2023, 951, 72; arXiv 2022, arXiv:2208.13582

    Pith/arXiv arXiv 2023

  22. [22]

    JWST NIRCam+NIRSpec: Interstellar medium and stellar populations of young galaxies with rising star fo r- mation and evolving gas reservoirs

    Tacchella, S.; Johnson, B.D.; Robertson, B.E.; Carniani, S.; D’Euge nio, F.; Kumar, N.; Maiolino, R.; Nelson, E.J.; Suess, K.A.; Übler, H.; et al . JWST NIRCam+NIRSpec: Interstellar medium and stellar populations of young galaxies with rising star fo r- mation and evolving gas reservoirs. arXiv 2022, arXiv:2208.03281

    Pith/arXiv arXiv 2022

  23. [23]

    The Identification of a Dusty Mu l- tiarm Spiral Galaxy at z = 3.06 with JWST and ALMA

    Wu, Y.; Cai, Z.; Sun, F.; Bian, F.; Lin, X.; Li, Z.; Li, M.; Bauer, F.E.; Egami, E.; Fan, X.; et al. The Identification of a Dusty Mu l- tiarm Spiral Galaxy at z = 3.06 with JWST and ALMA. arXiv 2022, arXiv:2208.08473

    Pith/arXiv arXiv 2022

  24. [24]

    Early Results from GLASS -JWST

    Yang, L.; Morishita, T.; Leethochawalit, N.; Castellano, M.; Calabro, A.; Treu, T.; Bonchi, A.; Fontana, A.; Mason, C.; Merlin, E.; et al. Early Results from GLASS -JWST. V: The First Rest -frame Optical Size–Luminosity Relation of Galaxies at z > 7 . Astrop- hys. J. Lett. 2022, 938, L17

    2022

  25. [25]

    A Large Population of Faint 8<z<16 Galaxies Found in the First JWST NIRCam Observations of the NGDEEP Survey

    Austin, D.; Adams, N.J.; Conselice, C.J.; Harvey, T.; Ormerod, K.; Trussler, J.; Li, Q.; Ferreira, L.; Dayal, P. A Large Population of Faint 8<z<16 Galaxies Found in the First JWST NIRCam Observations of the NGDEEP Survey. arXiv 2023, arXiv:2302.04270

    Pith/arXiv arXiv 2023

  26. [26]

    Sizes and Mass Profiles of Candidate Massive Galaxies Discovered by JWST at 7 < z < 9: Evidence for Very Early Formation of the Central ~100 pc of Present-day Ellipticals

    Baggen, J.F.W.; van Do kkum, P.; Labb é, I.; Brammer, G.; Miller, T.B.; Bezanson, R.; Leja, J.; Wang, B.; Whitaker, K.E.; Suess, K.A.; et al. Sizes and Mass Profiles of Candidate Massive Galaxies Discovered by JWST at 7 < z < 9: Evidence for Very Early Formation of the Central ~100 pc of Present-day Ellipticals. Astrophys. J. Lett. 2023, 955, L12

    2023

  27. [27]

    Efficient Formation of Massive Galaxies at Cosmic Dawn by Fee d- back-Free Starbursts

    Dekel, A.; Sarkar, K.S.; Birnboim, Y.; Mandelker, N.; Li, Z. Efficient Formation of Massive Galaxies at Cosmic Dawn by Fee d- back-Free Starbursts. arXiv 2023, arXiv:2303.04827

    Pith/arXiv arXiv 2023

  28. [28]

    A massive interacting galaxy 510 million years after the Big Bang arXiv 2023, arXiv:2303.00306

    Boyett, K.; Trenti, M.; Leethochawalit, N.; Calabró, A.B.; Roberts-Borsani, G.; et al. A massive interacting galaxy 510 million years after the Big Bang arXiv 2023, arXiv:2303.00306

    Pith/arXiv arXiv 2023

  29. [29]

    A recently quenched galaxy 700 million years after the Big Bang

    Looser, T.J.; D’Eugenio, F.; Maiolino, R.; Witstok, J.; Sandals, L.; Curtis-Lake, E.; Chevallard, J.; Tacchella, S.; Johnson, B.D.; Baker, W.M.; et al. A recently quenched galaxy 700 million years after the Big Bang. arXiv 2023, arXiv:2302.14155

    Pith/arXiv arXiv 2023

  30. [30]

    Efficient NIRCam Selection of Quiescent Galaxies at 3 < z < 6 in CEERS

    Long, A.S.; Antwi-Danso, J.; Lambrides, E.L.; Lovell, C.C.; de la Vega , A.; Valentino, F.; Zavala, J.A.; Casey, C.M.; Wilkins, S.M.; Yung, L.Y.A.; et al. Efficient NIRCam Selection of Quiescent Galaxies at 3 < z < 6 in CEERS. arXiv 2023, arXiv:2305.04662

    Pith/arXiv arXiv 2023

  31. [31]

    JADES NIRSpec Spectroscopy of GN-z11: Lyman-α emission and possible enhanced nitrogen abundance in a z = 10.60 luminous galaxy

    Bunker, A.J.; Saxena, A.; Cameron, A.J.; Willott, C.J.; Curtis -Lake, E.; Jakobsen, P.; Carniani, S.; Smit, R.; Maiolino, R.; Witstok, J.; et al. JADES NIRSpec Spectroscopy of GN-z11: Lyman-α emission and possible enhanced nitrogen abundance in a z = 10.60 luminous galaxy. arXiv 2023, arXiv:2302.07256. 16 of 22

    Pith/arXiv arXiv 2023

  32. [32]

    JADES Imaging of GN -z11: Revealing the Morphology and Environment of a Luminous Galaxy 430 Myr After the Big Bang

    Tacchella, S.; Eisenstein, D.J.; Hainline, K.; Johnson, B.D.; Baker, W.M.; Helton, J.M.; Robertson, B.; Suess, K.A.; Chen, Z.; Nel- son, E.; et al . JADES Imaging of GN -z11: Revealing the Morphology and Environment of a Luminous Galaxy 430 Myr After the Big Bang. arXiv 2023, arXiv:2302.07234

    Pith/arXiv arXiv 2023

  33. [33]

    Haro, P.A.; Dickinson, M.; Finkelstein, S.L.; Fujimoto , S.; Fernandez, V.; Kartaltepe, J.S.; Jung, I.; Cole, J.W.; Burgarella, D.; Chworowsky, K. ; et al. Spectroscopic confirmation of CEERS NIRCam -selected galaxies at z ≃ 8–10. arXiv 2023, arXiv:2304.05378

    Pith/arXiv arXiv 2023

  34. [34]

    Has JWST Already Falsified Dark -matter-driven Galaxy Formation? As- trophys

    Haslbauer, M.; Kroupa, P.; Zonoozi, A.H.; Haghi, H. Has JWST Already Falsified Dark -matter-driven Galaxy Formation? As- trophys. J. Lett. 2022, 939, L31

    2022

  35. [35]

    A Lower Bound of Star Formation Activity in Ultra -high-redshift Gal- axies Detected with JWST: Implications for Stellar Populations and Radiation Sources

    Inayoshi, K.; Harikane, Y.; Inoue, A.K.; Li, W.; Ho, L.C. A Lower Bound of Star Formation Activity in Ultra -high-redshift Gal- axies Detected with JWST: Implications for Stellar Populations and Radiation Sources. Astrophys. J. Lett. 2022, 938, L10

    2022

  36. [36]

    The MillenniumTNG Project: The galaxy population at z ≥ 8

    Kannan, R.; Springel, V.; Hernquist, L.; Pakmor, R.; Delgado, A.M.; Hadzhiyska, B.; Hernández -Aguayo, C.; Barrera, M.; Ferlito, F.; Bose, S.; et al. The MillenniumTNG Project: The galaxy population at z ≥ 8. arXiv 2022, arXiv:2210.10066

    Pith/arXiv arXiv 2022

  37. [37]

    Can Cosmological Simulations Reproduce the Spectroscopically Co n- firmed Galaxies Seen at z ≥ 10? arXiv 2022, arXiv:2212.12804

    Keller, B.W.; Muns hi, F.; Trebitsch, M.; Tremmel, M. Can Cosmological Simulations Reproduce the Spectroscopically Co n- firmed Galaxies Seen at z ≥ 10? arXiv 2022, arXiv:2212.12804

    Pith/arXiv arXiv 2022

  38. [38]

    Massive Star Formation in Overdense Regions of the Early Universe

    Regan, J. Massive Star Formation in Overdense Regions of the Early Universe. arXiv 2022, arXiv:2210.04899

    Pith/arXiv arXiv 2022

  39. [39]

    arXiv 2022, arXiv:2211.12970

    Yajima, H.; Abe, M.; Fukushima, H.; Ono, Y.; Harikane, Y.; Ouchi, M.; Hashimoto, T.; Khochfar, S.; FOREVER22: The first bright galaxies with population III stars at redshifts z ≃ 10–20 and comparisons with JWST data. arXiv 2022, arXiv:2211.12970

    Pith/arXiv arXiv 2022

  40. [40]

    JWST UNCOVER: Discovery of z > 9 Galaxy Candidates Behind the Lensing Cluster Abell 2744

    Atek, H.; Chemerynska, I.; Wang, B.; Furtak, L.; Weibel, A.; Oesch, P.; Weaver, J.R.; Labbé, I.; Bezanson, R.; van Dokkum, P.; et al. JWST UNCOVER: Discovery of z > 9 Galaxy Candidates Behind the Lensing Cluster Abell 2744 . arXiv 2023, arXiv:2305.01793

    Pith/arXiv arXiv 2023

  41. [41]

    The brightest galaxies at cosmic dawn

    Mason, C.A.; Trenti, M.; Treu, T. The brightest galaxies at cosmic dawn. Mon. Not. R. Astron. Soc. 2023, 521, 497

    2023

  42. [42]

    Balancing the efficiency and stochasticity of star formation with dust extinction in z ≳ 10 galaxies observed by JWST

    Mirocha, J.; Furlanetto, S.R. Balancing the efficiency and stochasticity of star formation with dust extinction in z ≳ 10 galaxies observed by JWST. Mon. Not. R. Astron. Soc. 2023, 519, 843

    2023

  43. [43]

    On the ages of bright galaxies ~500 Myr after the big bang: Insights into star formation activity at z ≳ 15 with JWST

    Whitler, L.; Endsley, R.; Stark, D.P.; Topping, M.; Chen, Z.; Charlot, S. On the ages of bright galaxies ~500 Myr after the big bang: Insights into star formation activity at z ≳ 15 with JWST. Mon. Not. R. Astron. Soc. 2023, 519, 157

    2023

  44. [44]

    Eilers, A.-C.; Simcoe, R.A.; Yue, M.; Mackenzie, M.Y.R.; Matthee, J.; Durovcikova, D.; Kashino, D.; Bordoloi, R.; Lilly, S.J. EI- GER. V. Characterizing the host galaxies of luminous quasars at z ≳ 6. Astrophys. J. 2023, 950, 67

    2023

  45. [45]

    A grand -design spiral galaxy 1.5 billion years after the Big Bang with JWST

    Jain, R.; Wadadekar, Y. A grand -design spiral galaxy 1.5 billion years after the Big Bang with JWST. arXiv 2024, arXiv:2412.04834

    arXiv 2024

  46. [46]

    When Galaxies Were Born: The Quest for Cosmic Dawn; Princeton University Press: Princeton, NJ, USA, 2022

    Ellis, R.S. When Galaxies Were Born: The Quest for Cosmic Dawn; Princeton University Press: Princeton, NJ, USA, 2022

    2022

  47. [47]

    Formation of supermassive stars in the first star clusters

    Bastian, R.; Klessen, R.S.; Schleicher, D.; Glover, S.C.O.; Solar, P. Formation of supermassive stars in the first star clusters. Mon. Not. R. Astron. Soc. 2023, 521, 3553–3569

    2023

  48. [48]

    Infe rred galaxy properties during Cosmic Dawn from early JWST photometry results

    Brummel-Smith, C.; Skinner, D.; Sethuram, S.S.; Wise, J.H.; Xia, B.; Taori, K. Infe rred galaxy properties during Cosmic Dawn from early JWST photometry results. arXiv 2023, arXiv:2302.04882

    Pith/arXiv arXiv 2023

  49. [49]

    The most massive Population III stars

    Chantavat, T.; Chongchitnan, S.; Silk, J. The most massive Population III stars. arXiv 2023, arXiv:2302.09763

    Pith/arXiv arXiv 2023

  50. [50]

    James Webb Space Telescope: Data, problems, and resolution

    Dolgov, A.D. James Webb Space Telescope: Data, problems, and resolution. arXiv 2023, arXiv: 2301.01365

    Pith/arXiv arXiv 2023

  51. [51]

    Larson, R.L.; Finkelstein, S.L.; Kocevski, D.D.; Hutchison, T.A.; et. Al. A CEERS Discovery of an Accreting Supermassive Blac k Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars. arXiv 2023, arXiv:2303.08918

    Pith/arXiv arXiv 2023

  52. [52]

    A small and vigorous black hole in the early Universe

    Maiolino, R.; Scholtz, J.; Witstok, J.; Carniani, S.; D'Eugenio, F.; de Graaff, A.; Uebler, H.; Tacchella, S.; Curtis-Lake, E.; Arribas, S.; et al. A small and vigorous black hole in the early Universe. arXiv 2023, arXiv:2305.12492

    Pith/arXiv arXiv 2023

  53. [53]

    Stress testing ΛCDM with high -redshift galaxy candidates

    Boylan-Kolchin, M. Stress testing ΛCDM with high -redshift galaxy candidates. Nat. Astron. 2023, 7, 731. https://doi.org/10.1038/s41550-023-01937-7

    doi:10.1038/s41550-023-01937-7 2023

  54. [54]

    Evidence for a Shallow Evolution in the Volume Densities of Massive Galaxies at z = 4 –8 from CEERS

    Chworowsky, K.; Finkelstein, S.L.; Boylan -Kolchin, M.; McGrath, E.J.; Iyer, K.G .; Papovich, C.; Dickinson, M.; Taylor, A.J.; Yung, L.Y.A.; Haro, R.A.; et al. Evidence for a Shallow Evolution in the Volume Densities of Massive Galaxies at z = 4 –8 from CEERS. Astron. J. 2024, 168, 113. https://doi.org/10.3847/1538-3881/ad57c1

    doi:10.3847/1538-3881/ad57c1 2024

  55. [55]

    Harvey, T.; Conselice, C.J.; Adams, N.J.; Austin, D.; Juodžbalis, I.; Trussler, J.; Li, Q.; Ormerod, K.; Ferreira, L.; Lovell, C.C.; et al. EPOCHS. IV. SED Modeling Assumptions and Their Impact on the Stellar Mass Function at 6.5 ≤ z ≤ 13.5 Using PEARLS and Public JWST Observations. Astrophys. J. 2025, 978, 89

    2025

  56. [56]

    Are we surprised to find SMBHs with JWST at z > 9? arXiv 2023, arXiv:2305.12504

    Schneider, R.; Valiante, R.; Trinca, A.; Graziani, L.; Volonteri, M.; Maiolino, R. Are we surprised to find SMBHs with JWST at z > 9? arXiv 2023, arXiv:2305.12504. 17 of 22

    Pith/arXiv arXiv 2023

  57. [57]

    The Relationship between St ellar Light Distributions of Galaxies and Their Formation Histories

    Conselice, C.J. The Relationship between St ellar Light Distributions of Galaxies and Their Formation Histories . Astrophys. J. Suppl. Ser. 2003, 147, 1. https://doi.org/10.1086/375001

    doi:10.1086/375001 2003

  58. [58]

    A New Nonparametric Approach to Galaxy Morphological Classification

    Lotz, J.M.; Primack, J.; Madau, P. A New Nonparametric Approach to Galaxy Morphological Classification . Astron. J. 2004, 128, 163. https://doi.org/10.1086/421849

    doi:10.1086/421849 2004

  59. [59]

    How was the Hubble sequence 6 Gyr ago? Astron

    Delgado-Serrano, R.; Hammer, F.; Yang, Y.B.; Puech, M.; Flores, H.; Rodrigues, M. How was the Hubble sequence 6 Gyr ago? Astron. Astrophys. 2010, 509, A78. https://doi.org/10.1051/0004-6361/200912704

    doi:10.1051/0004-6361/200912704 2010

  60. [60]

    The redshift and mass dependence on the formation of the Hubble sequence at z > 1 from CANDELS/UDS Free

    Mortlock, A.; Conselice, C.J.; Hartley, W.G.; Ownsworth, J.R.; Lani, C.; Bluck, A.F.L.; Almaini, O.; Duncan, K.; van der Wel, A.; Koekemoer, A.M. The redshift and mass dependence on the formation of the Hubble sequence at z > 1 from CANDELS/UDS Free. Mon. Not. R. Astron. Soc. 2013, 433, 1185. https://doi.org/10.1093/mnras/stt793

    doi:10.1093/mnras/stt793 2013

  61. [61]

    Early-type galaxies have been the predominant morphological class for massive galaxies since only z ∼ 1 Mon

    Buitrago F.; Trujillo, I.; Conselice, C.J.; Häußler, B. . Early-type galaxies have been the predominant morphological class for massive galaxies since only z ∼ 1 Mon. Not. R. Astron. Soc. 2013, 428, 1460

    2013

  62. [62]

    The Evolution of Galaxy Structure over Cosmic Time ; Annual Reviews Inc

    Conselice, C.J. The Evolution of Galaxy Structure over Cosmic Time ; Annual Reviews Inc. : San Mateo, CA, USA, 2014. https://doi.org/10.1146/annurev-astro-081913-040037

    doi:10.1146/annurev-astro-081913-040037 2014

  63. [63]

    The green valley is a red herring: Galaxy Zoo reveals two evolutionary pathways towards quenching of star fo r- mation in early- and late-type galaxies

    Schawinski, K.; Urry, C.M.; Simmons, B.D.; Fortson, L.; Kaviraj, S.; Keel, W.C.; Lintott, C.J.; Masters, K.L.; Nichol, R.C.; Sarzi, M.; et al . The green valley is a red herring: Galaxy Zoo reveals two evolutionary pathways towards quenching of star fo r- mation in early- and late-type galaxies. Mon. Not. R. Astron. Soc. 2014, 440, 889. https://doi.org/10...

    doi:10.1093/mnras/stu327 2014

  64. [64]

    Galaxy Evolution in All Five CANDELS Fields and IllustrisTNG: Mo r- phological, Structural, and the Major Merger Evolution to z ~ 3

    Whitney, A.; Ferreira, L.; Conselice, C.J.; Duncan, K. Galaxy Evolution in All Five CANDELS Fields and IllustrisTNG: Mo r- phological, Structural, and the Major Merger Evolution to z ~ 3. Astrophys. J. 2021, 919, 139. https://doi.org/10.3847/1538-4357/ac1422

    doi:10.3847/1538-4357/ac1422 2021

  65. [65]

    Early Results from GLASS -JWST

    Castellano, M.; Fontana, A.; Treu, T.; Santini, P.; Merlin, E.; Leethochawalit, N.; Trenti, M.; Vanzella, E.; Mestric, U.; Bo nchi, A.; et al. Early Results from GLASS -JWST. III. Galaxy Candidates at z 9 -15. Astrophys. J. 2022, 938, L15. https://doi.org/10.3847/2041-8213/ac94d0

    doi:10.3847/2041-8213/ac94d0 2022

  66. [66]

    CEERS Key Paper

    Finkelstein, S.L.; Bagley, M.B.; Ferguson, H.C.; Wilkins, S.M.; Kartaltepe, J.S.; Papovich, C.; Yung, L.Y.A.; Haro, P.A.; Behroozi, P.; Dickinson, M.; et al. CEERS Key Paper. I. An Early Look into the First 500 Myr of Galaxy Formation with JWST . Astrophys. J. 2023, 946, L13. https://doi.org/10.3847/2041-8213/acade4

    doi:10.3847/2041-8213/acade4 2023

  67. [67]

    First Batch of z ≈ 11–20 Candidate Objects Revealed by the James Webb Sp a- ce Telescope Early Release Observations on SMACS 0723 -73

    Yan, H.; Ma, Z.; Ling, C.; Cheng, C.; Huang, J.-S. First Batch of z ≈ 11–20 Candidate Objects Revealed by the James Webb Sp a- ce Telescope Early Release Observations on SMACS 0723 -73. Astrophys. J. 2022, 942, L9. https://doi.org/10.3847/2041-8213/aca80c

    doi:10.3847/2041-8213/aca80c 2022

  68. [68]

    The JWST Hubble Sequence: The Rest-Frame Optical Evolution of Galaxy Structure at 1.5 > z > 8

    Ferreira, L.; Conselice, C.J.; Sazonova, E.; Ferrari, F.; Caruana, J.; Tohill, C.; Lucatelli, G.; Adams, N.; Irodotou, D.; Marshall, M.A.; et al. The JWST Hubble Sequence: The Rest-Frame Optical Evolution of Galaxy Structure at 1.5 > z > 8. Astrophys. J. 2022, 955, 15

    2022

  69. [69]

    Panic! at the Disks: First Rest -frame Optical Observations of Galaxy Structure at z > 3 with JWST in the SMACS 0723 Field

    Ferreira, L.; Adams, N.; Conselice, C.J.; Sazonova, E.; Austin, D.; Caruana, J.; Ferrari, F.; Verma, A.; Trussler, J.; Broadhurst, T.; et al. Panic! at the Disks: First Rest -frame Optical Observations of Galaxy Structure at z > 3 with JWST in the SMACS 0723 Field. Astrophys. J. 2022, 938, L2. https://doi.org/10.3847/2041-8213/ac947c

    doi:10.3847/2041-8213/ac947c 2022

  70. [70]

    Early Results from GLASS -JWST

    Jacobs, C.; Glazebrook, K.; Calabrò, A.; Treu, T.; Nannayakkara, T.; Jones, T.; Merlin, E.; Abraham, R.; Stevens, A.R.H.; Vulc a- ni, B.; et al. Early Results from GLASS -JWST. XVIII. A First Morphological Atlas of the 1 < z < 5 Universe in the Rest -frame Optical. Astrophys. J. 2023, 948, L13. https://doi.org/10.3847/2041-8213/accd6d

    doi:10.3847/2041-8213/accd6d 2023

  71. [71]

    Recent observations of the rotation of distant galaxies and the implication for dark matter

    Nelson, A.H.; Williams, P.R. Recent observations of the rotation of distant galaxies and the implication for dark matter. Astron. Astrophys. 2024, 687, A261

    2024

  72. [72]

    Morpheus Reveals Distant Disk Galaxy Morphologies with JWST: The First AI/ML Analysis of JWST Images

    Robertson, B.E.; Tacchella, S.; Johnson, B.D.; Hausen, R.; Alabi, A.B.; Boyett, K.; Bunker, A.J.; Carniani, S.; Egami, E.; Eisenstein, D.J.; et al . Morpheus Reveals Distant Disk Galaxy Morphologies with JWST: The First AI/ML Analysis of JWST Images . As- trophys. J. 2023, 942, L42. https://doi.org/10.3847/2041-8213/aca086

    doi:10.3847/2041-8213/aca086 2023

  73. [73]

    EPOCHS XI: The Structure and Morphology of Galaxies in the Epoch of Reionization to z ~ 12.5

    Westcott, L.; Conselice, C.J.; Harvey, T.; Austin, D.; Adams, N.; Ferrari, F.; Ferreira, L.; Trussler, J.; Li, Q.; Rusakov, V .; et al. EPOCHS XI: The Structure and Morphology of Galaxies in the Epoch of Reionization to z ~ 12.5. arXiv 2024, arXiv:2412.14970. https://doi.org/10.48550/arXiv.2412.14970

    Pith/arXiv arXiv doi:10.48550/arxiv.2412.14970 2024

  74. [74]

    Strong size evolution of the most massive gala x- ies since z ~ 2

    Trujillo, I.; Conselice, C.J.; Bundy, K.; Cooper, M.C.; Eisenhardt, P.; Ellis, R.S. Strong size evolution of the most massive gala x- ies since z ~ 2. Mon. Not. R. Astron. Soc. 2007, 382, 109. https://doi.org/10.1111/j.1365-2966.2007.12388.x

    arXiv 2007

  75. [75]

    Size Evolution of the Most Massive Galaxie s at 1.7 < z < 3 from GOODS NICMOS Survey Imaging

    Buitrago, F.; Trujillo, I.; Conselice, C.J.; Bouwens, R.J.; Dickinson, M.; Yan, H. Size Evolution of the Most Massive Galaxie s at 1.7 < z < 3 from GOODS NICMOS Survey Imaging. Astrophys. J. 2008, 687, L61. https://doi.org/10.1086/592836. 18 of 22

    doi:10.1086/592836 2008

  76. [76]

    Structural Parameters of Galaxies in Candels

    van der Wel, A.; Bell, E.F.; Häussler, B.; McGrath, E.J.; Chang, Y.-Y.; Guo, Y.; McIntosh, D.H.; Rix, H.-W.; Barden, M.; Cheung, E.; et al. Structural Parameters of Galaxies in Candels . Astrophys. J. Suppl. Ser. 2012, 203, 24. https://doi.org/10.1088/0067-0049/203/2/24

    doi:10.1088/0067-0049/203/2/24 2012

  77. [77]

    EPOCHS VI: The size and shape evolution of galaxies since z ~ 8 with JWST Observations

    Ormerod, K.; Conselice, C.J.; Adams, N.J.; Harvey, T.; Austin, D.; Trussler, J.; Ferreira, L.; Caruana, J.; Lucatelli, G.; Li, Q.; et al. EPOCHS VI: The size and shape evolution of galaxies since z ~ 8 with JWST Observations. Mon. Not. R. Astron. Soc. 2024, 527,

    2024

  78. [78]

    Whitaker, K.E.; Brammer, G

    van Dokkum, P.G. ; Whitaker, K.E.; Brammer, G. ; Franx, M.; Kriek, M.; Labbé, I.; Marchesini, D.; Quadri, R.; Bezanson, R.; Illingworth, G.D.; et al . The Growth of Massive Galaxies Since z = 2 . Astrophys. J. 2010, 709, 1018. https://doi.org/10.1088/0004-637X/709/2/1018

    doi:10.1088/0004-637x/709/2/1018 2010

  79. [79]

    Expectations of the Size Evolution of Massive Galaxies at 3 ≤ z ≤ 6 from the TNG50 Simulation: The CEERS/JWST View

    Costantin, L.; Pérez-González, P.G.; Vega-Ferrero, J.; Huertas-Company, M.; Bisigello, L.; Buitrago, F.; Bagley, M.B.; Cleri, N.J.; Cooper, M.C.; Finkelstein, S.L.; et al. Expectations of the Size Evolution of Massive Galaxies at 3 ≤ z ≤ 6 from the TNG50 Simulation: The CEERS/JWST View. Astrophys. J. 2023, 946, 71. https://doi.org/10.3847/1538-4357/acb926

    doi:10.3847/1538-4357/acb926 2023

  80. [80]

    The sizes of bright Lyman -break galaxies at 𝑧 ≅ 3 − 5 with JWST PRIMER

    Varadaraj, R.G.; Bowler, R.A.A.; Jarvis, M.J.; Adams, N.J.; Choustikov, N.; Koekemoer, A.M.; Carnall, A.C.; McLeod, D.J.; Dunlop, J.S.; Donnan, C.T.; Grogin, N.A. The sizes of bright Lyman -break galaxies at 𝑧 ≅ 3 − 5 with JWST PRIMER.. arXiv 2024, arXiv: 2401.15971

    Pith/arXiv arXiv 2024

Showing first 80 references.