Pith. sign in

REVIEW 4 major objections 4 minor 199 references

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

T0 review · 4 major / 4 minor · reviewed 2026-08-04 · deepseek-v4-flash

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

desk verdict 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. read the letter →

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

classification physics.gen-ph
keywords galaxyevolutionhigh-redshiftgalaxiesearlyuniversetiredlightcovaryingcouplingconstantsangulardiameterdistanceJWSTsize-mass-densityrelation
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 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.

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.

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

Extended reading notes

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,

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.

Editorial extensions

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.

Reading between the lines

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.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, 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 · score 7.0 of 10

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.

  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.

Assumptions & free parameters 2 free parameters · 6 assumptions · 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.
assumptions (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
    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.
    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.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Evolution of Size, Mass, and Density of Galaxies Since Cosmic Dawn." pith.science (2026). https://pith.science/paper/XEKXVJQE

@misc{pith2026251013844,
  author       = {Pith},
  title        = {Pith review of: Evolution of Size, Mass, and Density of Galaxies Since Cosmic Dawn},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/XEKXVJQE}},
  note         = {Machine review of arXiv:2510.13844}
}
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 the authors.

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. 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 ΛCDM framew… view at source ↗
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 hole mass i… view at source ↗
Figures from the paper (3 more)
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]
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.…
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 dynam…

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

199 extracted references · 1 canonical work pages

  1. [86]

    JWST early Universe observations and ΛCDM cosmology

    Gupta, R.P. JWST early Universe observations and ΛCDM cosmology. Mon. Not. R. Astron. Soc. 2023, 524, 3385

  2. [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

  3. [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

  4. [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

  5. [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

  6. [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

  7. [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

  8. [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

Show all 199 references
  1. [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

  2. [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. M...

  3. [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

  4. [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...

  5. [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–...

  6. [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

  7. [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 ...

  8. [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, ...

  9. [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. 20...

  10. [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

  11. [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

  12. [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....

  13. [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. Astrophy...

  14. [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...

  15. [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...

  16. [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

  17. [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. 202...

  18. [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

  19. [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...

  20. [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

  21. [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

  22. [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

  23. [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

  24. [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. arX...

  25. [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, ...

  26. [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

  27. [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

  28. [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

  29. [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

  30. [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

  31. [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

  32. [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

  33. [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

  34. [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

  35. [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

  36. [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

  37. [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

  38. [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

  39. [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

  40. [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

  41. [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

  42. [49]

    The most massive Population III stars

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

  43. [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

  44. [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

  45. [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

  46. [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

  47. [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,...

  48. [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 Observa...

  49. [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

  50. [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

  51. [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

  52. [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

  53. [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. ...

  54. [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

  55. [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

  56. [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 ...

  57. [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

  58. [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

  59. [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. ...

  60. [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

  61. [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

  62. [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. ...

  63. [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. ...

  64. [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

  65. [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...

  66. [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/1...

  67. [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

  68. [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

  69. [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

  70. [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,

  71. [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

  72. [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/...

  73. [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

  74. [81]

    The Size Evolution and the Size -Mass Relation of Ly- man-Alpha Emitters across 3 ≤ 𝑧 < 7 as Observed by JWST

    Song, Q.; Liu, F.S.; Ren, J.; Zhao, P.; Cui, W.; Li, Y.; Mo, H.; Luo, Y.; et al. The Size Evolution and the Size -Mass Relation of Ly- man-Alpha Emitters across 3 ≤ 𝑧 < 7 as Observed by JWST. arXiv 2025, arXiv:2508.05052

  75. [82]

    COSMOS-Web: Unraveling the Evolution of Galaxy Size and Related Properties at 2 < z < 10

    Yang, L.; Kartaltepe, J.S.; Franco, M.; Ding, X.; Achenbach, M.J.; Arango-Toro, R.C.; Casey, C.M.; Drakos, N.E.; Faisst, A.L.; Gillman, S.; et al. COSMOS-Web: Unraveling the Evolution of Galaxy Size and Related Properties at 2 < z < 10. arXiv 2025, ar- Xiv:2504.07185

  76. [83]

    Evolution of the Size –Mass Relation of Star -forming Galaxies Since z = 5.5 Revealed by CEERS

    Ward, E.; de la Vega, A.; Mobasher, B.; McGrath, E.J.; Iyer, K.G .; Calabrò, A.; Costantin, L.; Dickinson, M.; Holwerda, B.W.; Huertas-Company, M.; et al. Evolution of the Size –Mass Relation of Star -forming Galaxies Since z = 5.5 Revealed by CEERS. Astrophys. J. 2024, 962, 1...

  77. [84]

    Varying Coupling Constants and Their Interdependence

    Gupta, R.P. Varying Coupling Constants and Their Interdependence. Mod. Phys. Lett. A 2022, 37, 2250155; arXiv: 2201.11667 (corrected version)

  78. [85]

    O n The Red Shift of Spectral Lines Through Interatellar Space

    Zwicky, F. O n The Red Shift of Spectral Lines Through Interatellar Space. Proc. Natl. Acad. Sci. USA 1929, 15, 77 3. https://doi.org/10.1073/pnas.15.10.773

  79. [87]

    Testing CCC+TL Cosmology with Observed BAO Features

    Gupta, R.P. Testing CCC+TL Cosmology with Observed BAO Features. Astrophys. J. 2024, 964, 55

  80. [88]

    On Dark Matter and Dark Energy in CCC+TL Cosmology

    Gupta, R.P. On Dark Matter and Dark Energy in CCC+TL Cosmology. Universe 2024, 10, 266

  81. [89]

    Testing CCC+TL Cosmology with Galaxy Rotation Curves

    Gupta, R.P. Testing CCC+TL Cosmology with Galaxy Rotation Curves. Galaxies 2025, 13, 108

  82. [90]

    Very Metal-poor Stars in the Solar Vicinity: Age Determination

    Plotnikova, A.; Carraro, G.; Villanova, S.; Ortolani, S. Very Metal-poor Stars in the Solar Vicinity: Age Determination . Astrop- hys. J. 2022, 940, 159

  83. [91]

    Some Old Globular Clusters (and Stars) Inferring That the Universe Is Older Than Commonly Accepted

    de Andrés, F.L. Some Old Globular Clusters (and Stars) Inferring That the Universe Is Older Than Commonly Accepted. arXiv 2024, arXiv:2401.11549

  84. [92]

    The Cosmological Constants

    Dirac, P.A.M. The Cosmological Constants. Nature 1937, 139, 323

  85. [93]

    Varying Constants, Gravitation and Cosmology

    Uzan, J.-P. Varying Constants, Gravitation and Cosmology. Living Rev. Relativ. 2011, 14, 2

  86. [94]

    On the Change of Physical Constants

    Teller, E. On the Change of Physical Constants. Phys. Rev. 1948, 73, 801

  87. [95]

    Limit on the Secular Change of the Gravitational Constant Based on Studies of Solar Evolution

    Chin, C.-w.; Stothers, R. Limit on the Secular Change of the Gravitational Constant Based on Studies of Solar Evolution. Phys. Rev. Lett. 1976, 36, 833

  88. [96]

    Can a variable gravitational constant resolve the faint young Sun paradox? Int

    Sahini, V.; Shtanov, Y. Can a variable gravitational constant resolve the faint young Sun paradox? Int. J. Mod. Phys. D 2014, 23, 1442018

  89. [97]

    Rotation of the Earth from AD 1663–1972 and the Constancy of G

    Morrison, L.V. Rotation of the Earth from AD 1663–1972 and the Constancy of G. Nature 1973, 241, 519

  90. [98]

    Cosmology, oscillating physics, and oscillating biology

    Sisterna, P.D.; Vucetich, H. Cosmology, oscillating physics, and oscillating biology. Phys. Rev. Lett. 1994, 72, 454

  91. [99]

    Torres, D.F

    Benvenuto, O.G.; A lthaus, L.G. ; Torres, D.F. Evolution of white dwarfs as a probe of theories of gravitation: The case of Brans—Dicke. Mon. Not. R. Astron. Soc. 1999, 305, 905

  92. [100]

    An upper limit to the s ecular variation of the gravitati o- nal constant from white dwarf stars

    Garcia-Berro, E.; Lorén-Aguilar, P.; Torres, S.; Althaus, L.G.; Isern, J. An upper limit to the s ecular variation of the gravitati o- nal constant from white dwarf stars. J. Cosmol. Astropart. Phys. 2011, 05, 021

  93. [101]

    An independent constraint on the secular rate of variation of the gravitational constant from pulsating white dwarfs

    Corsico, A.H.; Althaus, L.G.; García-Berro, E.; Romero, A.D. An independent constraint on the secular rate of variation of the gravitational constant from pulsating white dwarfs. J. Cosmol. Astropart. Phys. 2013, 06, 032. 19 of 22

  94. [102]

    Time-Variation of Newton's Constant and the Age of Glo b- ular Clusters

    Degl’Innocenti, S.; Fiorentini, G.; Raffelt, G.G.; Ricci, B.; Weiss, A. Time-Variation of Newton's Constant and the Age of Glo b- ular Clusters. Astron. Astrophys. 1995, 312, 345

  95. [103]

    The Gravitational Constant, the Chandrasekhar Limit, and Neutron Star Masses

    Thorsett, S.E. The Gravitational Constant, the Chandrasekhar Limit, and Neutron Star Masses. Phys. Rev. Lett. 1996, 77, 1432

  96. [104]

    Cosmological constraints on the gravitational interactions of matter and dark matter

    Bai, Y.; Salvado, J.; Stefanek, B.A. Cosmological constraints on the gravitational interactions of matter and dark matter . J. Cos- mol. Astropart. Phys. 2015, 15, 029

  97. [105]

    Cosmological constraints on scalar–tensor gravity and the variation of the gravita- tional constant

    Ooba, J.; Ichiki, K.; Chiba, T.; Sugiyama, N. Cosmological constraints on scalar–tensor gravity and the variation of the gravita- tional constant. Prog. Theor. Exp. Phys. 2017, 2017, 043E03

  98. [106]

    New Nucleosynthesis Constraint on the Variation of 𝐺

    Copi, C.J.; Davis, A.N.; Krauss, L.M. New Nucleosynthesis Constraint on the Variation of 𝐺. Phys. Rev. Lett. 2004, 92, 171301

  99. [107]

    Improved BBN constraints on the variation of the gravitational constant

    Alvey, J.; Sabti, N.; Escudero, M.; Fairbairn, M. Improved BBN constraints on the variation of the gravitational constant . Eur. Phys. J. C 2020, 80, 148

  100. [108]

    Asteroseismic Constraints on the Cosmic -time Variation of the Gravitational Co n- stant from an Ancient Main-sequence Star

    Bellinger, E.P.; Christensen-Dalsgaard, J. Asteroseismic Constraints on the Cosmic -time Variation of the Gravitational Co n- stant from an Ancient Main-sequence Star. Astrophys. J. Lett. 2019, 887, L1

  101. [109]

    Progress in Lunar Laser Ranging Tests of Relativistic Gravity

    Williams, J.G.; Turyshev, S.G.; Boggs, D.H. Progress in Lunar Laser Ranging Tests of Relativistic Gravity. Phys. Rev. Lett. 2004, 93, 261101

  102. [110]

    Relativistic tests with lunar laser ranging

    Hofmann, F.; Müller, J. Relativistic tests with lunar laser ranging. Class. Quant. Grav. 2018, 35, 035015

  103. [111]

    Relativistic effects and dark matter in the Solar system from observations of planets and spacecraft

    Pitjeva, E.V.; Pitjev, N.P. Relativistic effects and dark matter in the Solar system from observations of planets and spacecraft . Mon. Not. R. Astron. Soc. 2013, 432, 3431

  104. [112]

    Tests of General relativity with planetary orbits and Monte Carlo simulations

    Fienga, A.; Laskar, J.; Exertier, P.; Manche, H.; Gastineau, M. Tests of General relativity with planetary orbits and Monte Carlo simulations. arXiv 2014, arXiv:1409.4932

  105. [113]

    Solar system expansion and strong equivalence principle as seen by the NASA MESSENGER misión

    Genova, A.; Mazarico, E.; Goossens, S.; Lemoine, F.G.; Neumann, G.A.; Smith, D.E.; Zuber, M.T. Solar system expansion and strong equivalence principle as seen by the NASA MESSENGER misión. Nat. Commun. 2018, 9, 289

  106. [114]

    Limits on the Variability of 𝐺 Using Binary-Pulsar Data

    Damour, T.; Gibbons, G.W.; Taylor, J.H. Limits on the Variability of 𝐺 Using Binary-Pulsar Data. Phys. Rev. Lett. 1988, 61, 1151

  107. [115]

    High -Precision Timing of Millisecond Pulsars

    Kaspi, V.M.; Taylor, J.H.; Ryba, M.F. High -Precision Timing of Millisecond Pulsars. III. Long -Term Monitoring of PSRs B1855+09 and B1937+21. Astrophys. J. 1994, 428, 713

  108. [116]

    Tests of gravitational symmetries with pulsar binary J1713+0747

    Zhu, W.W.; Desvignes, G.; Wex, N.; Caballero, R.N.; Champion, D.J.; Demorest, P.B.; Ellis, J.A.; Janssen, G.H.; Kramer, M.; Krieger, A.; et al. Tests of gravitational symmetries with pulsar binary J1713+0747. Mon. Not. R. Astron. Soc. 2019, 482, 3249

  109. [117]

    Bounds on the possible evolution of the gravitational cons- tant from cosmological type-Ia supernovae

    Gaztañaga, E.; García-Berro, E.; Isern, J.; Bravo, E.; Domínguez, I. Bounds on the possible evolution of the gravitational cons- tant from cosmological type-Ia supernovae. Phys. Rev. D 2001, 65, 023506

  110. [118]

    Type Ia supernovae, standardizable candles, and gravity

    Wright, B.S.; Li, B. Type Ia supernovae, standardizable candles, and gravity. Phys. Rev. D 2018, 97, 083505

  111. [119]

    Jahrbuch fur Radioaktivitat und Elektronik 4, 11

    Einstein, A. Jahrbuch fur Radioaktivitat und Elektronik 4, 11. 1907

  112. [120]

    Gravitation without a Principle of Equivalence

    Dicke, R.H. Gravitation without a Principle of Equivalence. Rev. Mod. Phys. 1957, 29, 363

  113. [121]

    An interpretation of cosmological model with variable light velocity

    Petit, J.-P. An interpretation of cosmological model with variable light velocity. Mod. Phys. Lett. A 1988, 3, 1527

  114. [122]

    Superluminary Universe: A Possible Solution to the Initial Value Problem in Cosmology

    Moffat, J.W. Superluminary Universe: A Possible Solution to the Initial Value Problem in Cosmology. Int. J. Mod. Phys. D 1993, 2, 351

  115. [123]

    Quantum gravity, the origin of time and time's arrow

    Moffat, J.W. Quantum gravity, the origin of time and time's arrow. Found. Phys. 1993, 23, 411

  116. [124]

    Time varying speed of light as a solution to cosmological puzzles

    Albrecht, A.; Magueijo, J. Time varying speed of light as a solution to cosmological puzzles. Phys. Rev. D 1999, 59, 043516

  117. [125]

    Cosmologies with varying light speed

    Barrow, J.D. Cosmologies with varying light speed. Phys. Rev. D 1999, 59, 043515

  118. [126]

    Does a varying speed of light solve the cosmological problems? Phys

    Avelino, P.P.; Martins, C.J.A.P. Does a varying speed of light solve the cosmological problems? Phys. Lett. B 1999, 459, 468

  119. [127]

    VSL theories and the Doppler peak

    Avelino, P.P.; Martins, C.J.A.P.; Rocha, G. VSL theories and the Doppler peak. Phys. Lett. B 2000, 483, 210

  120. [128]

    Variable speed of light cosmology, primordial fluctuations and gravitational waves

    Moffat, J.W. Variable speed of light cosmology, primordial fluctuations and gravitational waves. Eur. Phys. J. C 2016, 76, 130

  121. [129]

    Covariant c-flation: A variational approach

    Costa, R.; Cuzinatto, R.R.; Ferreira, E.G.M.; Franzmann, G. Covariant c-flation: A variational approach . Int. J. Mod. Phys. D 2019, 28, 1950119

  122. [130]

    Cosmology with relativistically varying physical constants, Mon

    Gupta, R.P. Cosmology with relativistically varying physical constants, Mon. Not. R. Astron. Soc. 2020, 498, 4481

  123. [131]

    Dynamical Analysis of the Covarying Coupling Constants in Scalar-Tensor Gravity

    Cuzinatto, R.R.; Gupta, R.P.; Pompeia, P.J. Dynamical Analysis of the Covarying Coupling Constants in Scalar-Tensor Gravity. Symmetry 2023, 15, 709

  124. [132]

    Covarying-Bi-Scalar Theory: A model with covarying G and c and a natural screening mechanism

    Cuzinatto, R.R.; Gupta , R.P.; Pompeia , P.J. Covarying-Bi-Scalar Theory: A model with covarying G and c and a natural screening mechanism. Ann. Phys. 2025, 479, 170039. https://doi.org/10.1016/j.aop.2025.170039

  125. [133]

    Cosmology in Scalar-Tensor Gravity; Springer: Berlin/Heidelberg, Germany, 2004; Chapter 2

    Faraoni, V. Cosmology in Scalar-Tensor Gravity; Springer: Berlin/Heidelberg, Germany, 2004; Chapter 2

  126. [134]

    Conformally Friedmann–Lemaître–Robertson–Walker cosmologies

    Visser, M. Conformally Friedmann–Lemaître–Robertson–Walker cosmologies. Class. Quant. Grav. 2015, 32, 135007

  127. [135]

    Cosmology in Minkowski space

    Lombriser, L. Cosmology in Minkowski space. Class. Quant. Grav. 2023, 40, 155005

  128. [136]

    Color-Mass-to-light-ratio Relations for Disk Galaxies

    McGaugh, S.S.; Schombert, J.M. Color-Mass-to-light-ratio Relations for Disk Galaxies. Astron. J. 2014, 148, 77. 20 of 22

  129. [137]

    Little Red Dots

    Baggen, J.F.W.; van Dokkum, P.; Brammer, G.; de Graaff, A.; Franx, M.; Greene, J.; Labbé, I.; Leja, J.; Maseda, M.V.; Nelson, E.J.; et al . The Small Sizes and High Implied Densities of “Little Red Dots” with Balmer Breaks Could Explain Their Broad Emission Lines without an Ac...

  130. [138]

    The stellar masses of galaxies from the 3.4 μm band of the WISE All-Sky Survey

    Wen, X.-Q.; Wu, H.; Zhu, Y.-N.; Lam, M.I.; Wu, C.-J.; Wicker, J.; Zhao, Y.-H. The stellar masses of galaxies from the 3.4 μm band of the WISE All-Sky Survey. Mon. Not. R. Astron. Soc. 2013, 433, 2946

  131. [139]

    Analysis of galaxy spectral energy distribu- tions from far-UV to far-IR with CIGALE: Studying a SINGS test sample

    Noll, S.; Burgarella, D.; Giovannoli, E.; Buat, V.; Marcillac, D.; Muñoz-Mateos, J.C. Analysis of galaxy spectral energy distribu- tions from far-UV to far-IR with CIGALE: Studying a SINGS test sample. Astron. Astrophys. 2009, 507, 1793

  132. [140]

    The imprint of rapid star formation quenching on the spectral energy distributions of galaxies

    Ciesla, L.; Boselli, A.; Elbaz, D.; Boissier, S.; Buat, V.; Charmandaris, V.; Schreiber, C.; Béthermin, M.; Baes, M.; Boquien, M.; et al. The imprint of rapid star formation quenching on the spectral energy distributions of galaxies. Astron. Astrophys. 2016, 585, A43

  133. [141]

    CIGALE: A python Code Investi- gating GALaxy Emission

    Boquien, M.; Burgarella, D.; Roehlly, Y.; Buat, V.; Ciesla, L.; Corre, D.; Inoue, A.K.; Salas, H. CIGALE: A python Code Investi- gating GALaxy Emission. Astron. Astrophys. 2019, 622, A103. https://doi.org/10.1051/0004-6361/201834156

  134. [142]

    Exploring the Nature of Little Red Dots: Constraints on AGN and Stellar Contributions from PRIMER MIRI Imaging

    Leung, G.C.K.; Finkelstein, S.L.; Perez-Gonzalez, P.G.; Morales, A.M.; Taylor, A.J.; Barro, G.; Kocevski, D.D.; Akins, H.B.; Carnall, A.C.; Ortiz, Ó.A.C.; et al. Exploring the Nature of Little Red Dots: Constraints on AGN and Stellar Contributions from PRIMER MIRI Imaging. arX...

  135. [143]

    Estimating Black Hole Masses in Active Galaxies Using the Hα Emission Line

    Greene, J.E.; Ho, L.C. Estimating Black Hole Masses in Active Galaxies Using the Hα Emission Line. Astrophys. J. 2005, 630,

  136. [144]

    The Rise of Faint, Red Active Galactic Nuclei at z > 4: A Sample of Little Red Dots in the JWST Extragalactic Legacy Fields

    Kocevski, D.D.; Finkelstein, S.L.; Barro, G.; Taylor, A.J.; Calabrò, A.; Laloux, B.; Buchner, J.; Trump, J.R.; Leung, G.C.K.; Yang, G.; et al. The Rise of Faint, Red Active Galactic Nuclei at z > 4: A Sample of Little Red Dots in the JWST Extragalactic Legacy Fields. arXiv 202...

  137. [145]

    https://doi.org/10.1086/431897

  138. [146]

    Deep Constraints on [CII]158 µm in JADES -GS-z14-0: Further Evidence for a Galaxy with Low G as Content at z=14.2

    Schouws, S.; Bouwens, R.J.; Algera, H.; Smit, R.; Kumari, N.; Rowland, L.E.; van Leeuwen, I.; Sommovigo, L.; Ferrara, A.; Oesch, P.A.; et al. Deep Constraints on [CII]158 µm in JADES -GS-z14-0: Further Evidence for a Galaxy with Low G as Content at z=14.2. arXiv 2025, arXiv:25...

  139. [147]

    Tentative detection of neutral gas in a Little Red Dot at z = 4.46

    Akins, H.B.; Casey, C.M.; Chisholm, J.; Berg, D.A.; Cooper, O.; Franco, M.; Fujimoto, S.; Lambrides, E.; Long, A.S.; McKinney, J. Tentative detection of neutral gas in a Little Red Dot at z = 4.46. arXiv 2025, arXiv :2503.00998. https://doi.org/10.48550/arXiv.2503.00998

  140. [148]

    Ultraviolet Compactness of High-Redshift Galaxies as a Tracer of Early -Stage Gas Infall, Bursty Star Formation, and Offset from the Fundamental Metallicity Relation

    Langeroodi, D.; Hjorth, J. Ultraviolet Compactness of High-Redshift Galaxies as a Tracer of Early -Stage Gas Infall, Bursty Star Formation, and Offset from the Fundamental Metallicity Relation. arXiv 2023, arXiv:2307.06336

  141. [149]

    Detection of [OIII]88 µm in JADES -GS-z14-0 at z = 14.1793

    Schouws, S.; Bouwens, R.J.; Ormerod, K.; Smit, R.; Algera, H.; Sommovigo, L.; Hodge, J.; Ferrara, A.; Oesch, P.A.; Rowland, L.E.; et al . Detection of [OIII]88 µm in JADES -GS-z14-0 at z = 14.1793. arXiv 2024, arXiv :2409.20549. https://doi.org/10.48550/arXiv.2409.20549

  142. [150]

    Westcott, L.; Conselice, C.J.; Harvey, T.; Austin, D.; Adams, N.; Ferrari, F.; et al. EPOCHS. XI. The Structure and Morphology of Galaxies in the Epoch of Reionization to z ∼ 12.5. Astrophys. J. 2025, 983, 121

  143. [151]

    Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe

    Langeroodi, D.; Hjorth, J.; Chen, W.; Kelly, P.L.; Williams, H.; Lin, Y.; Scarlata, C.; Zitrin, A.; Broadhurst, T.; Diego, J.M.; et al. Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe. Astrophys. J. 2023, 957, 39

  144. [152]

    On the Evolution of the Central Density of Quiescent Galaxies

    Tacchella, S.; Carollo, C.M.; Faber, S.M.; Cibinel, A.; Dekel, A.; Koo, D.C.; Renzini, A.; Woo, J. On the Evolution of the Central Density of Quiescent Galaxies. Astrophys. J. Lett. 2017, 844, L1

  145. [153]

    Feedback and dynamical masses in high-z galaxies: The advent of high-resolution NIRSpec spectroscopy arXiv 2025, arXiv:2501.17145

    Saldana-Lopez, A.; Chisholm, J.; Gazagnes, S.; Endsley, R.; Hayes, M.J.; Berg, D.A.; Finkelstein, S.L.; Flury, S.R.; Guseva, N.G.; Henry, A.; et al. Feedback and dynamical masses in high-z galaxies: The advent of high-resolution NIRSpec spectroscopy arXiv 2025, arXiv:2501.17145

  146. [154]

    The rise of the galactic empire: Luminosity functions at z ~ 7and z ~ 25 estimated with the MIDIS+NGDEEP ultra-deep JWST/NIRCam dataset

    Pérez-González, P.G.; Östlin, G.; Costantin, L.; Melinder, J.; Finkelstein, S.L.; Somerville, R.S.; Annunziatella, M.; Álva- rez-Márquez, J.; Colina, L.; Dekel, A.; et al. The rise of the galactic empire: Luminosity functions at z ~ 7and z ~ 25 estimated with the MIDIS+NGDEEP ...

  147. [155]

    del P.; et al

    Zhang, Y.; de Graaff, A.; Price, D.J.S.H.; Bezanson, R.; Lagos, C. del P.; et al. RUBIES spectroscopically confirms the high num- ber density of quiescent galaxies From 2 < 𝑧 < 5. arXiv 2025, arXiv:2508.08577

  148. [156]

    SAPPHIRES: A Galaxy Over-Density in the Heart of Cosmic Reionization at z = 8.47

    Fudamoto, Y.; Helton, J.M.; Lin, X.; Sun, F.; Behroozi, P.; Hsiao, T.Y.-Y.; Egami, E.; Bunker, A.J.; Harikane, Y.; Ouchi, M.; et al . SAPPHIRES: A Galaxy Over-Density in the Heart of Cosmic Reionization at z = 8.47. arXiv 2025, arXiv:2503.15597. 21 of 22

  149. [157]

    ALMA Band 3 Selection of Ultra-high Redshift Dropouts: The final challenge to ΛCDM

    Lovell, C.; Lee, M.; Vijayan, A.; Harvey, T.; Sommovigo, L.; Long, A.; Lambrides, E.; Roper, W.; Wilkins, S.; Narayanan, D.; et al. ALMA Band 3 Selection of Ultra-high Redshift Dropouts: The final challenge to ΛCDM. arXiv 2025, arXiv: 2503.24312

  150. [158]

    Unveiling the Cosmic Chemistry: Revisiting the Mass –Metallicity Relation with JWST/NIRSpec at 4 < z < 10

    Sarkar, A.; Chakraborty, P.; Vogelsberger, M.; McDonald, M.; Torrey, P.; Garcia, A.M.; Khullar, G.; Ferland, G.J.; Forman, W.; Wolk, S.; et al . Unveiling the Cosmic Chemistry: Revisiting the Mass –Metallicity Relation with JWST/NIRSpec at 4 < z < 10 . Astrophys. J. 2025, 978, 136

  151. [159]

    Witnessing the onset of reionization through Lyman -α emission at redshift 13

    Witstok, J.; Jakobsen, P.; Maiolino, R.; Helton, J.M.; Johnson, B.D.; Robertson, B.E.; Tacchella, S.; Cameron, A.J.; Smit, R.; Bun- ker, A.J.; et al. Witnessing the onset of reionization through Lyman -α emission at redshift 13 . Nature 2025, 639, 897 –901. https://doi.org/10....

  152. [160]

    A JWST/NIRSpec First Census of Broad-line AGNs at z = 4 –7: Detection of 10 F aint AGNs with M BH ~ 106–108M⊙ and Their Host Galaxy Properties

    Harikane, Y.; Zhang, Y.; Nakajima, K.; Ouchi, M.; Isobe, Y.; Ono, Y.; Hatano, S .; Xu, Y.; Umeda, H. A JWST/NIRSpec First Census of Broad-line AGNs at z = 4 –7: Detection of 10 F aint AGNs with M BH ~ 106–108M⊙ and Their Host Galaxy Properties. Astrophys. J. 2023, 959, 39. htt...

  153. [161]

    The eventful life of a luminous galaxy at z = 14: metal en- richment, feedback, and low gas fraction? Astron

    Carniani, S.; D’Eugenio, F.; Ji, X.; Parlanti1, E.; Scholtz, J.; Sun, F. The eventful life of a luminous galaxy at z = 14: metal en- richment, feedback, and low gas fraction? Astron. Astrophys. 2025, 696, A87

  154. [162]

    Little Red Dots: An Abundant Population of Faint Active Galactic Nuclei at z ~ 5 Revealed by the EIGER and FRESCO JWST Surveys

    Matthee, J.; Naidu, R.P.; Brammer, G.; Chisholm, J.; Eilers, A.-C.; Goulding, A.; Greene, J.; Kashino, D.; Labbe, I.; Lilly, S.J.; et al. Little Red Dots: An Abundant Population of Faint Active Galactic Nuclei at z ~ 5 Revealed by the EIGER and FRESCO JWST Surveys. Astrophys. ...

  155. [163]

    Broad-Line AGN at 3.5 < z < 6: The Black Hole Mass Function and a Connection with Little Red Dots

    Taylor, A.J.; Finkelstein, S.L.; Kocevski, D.D.; Jeon, J.; Bromm, V.; Amorin, R.O.; Haro, P.A.; Backhaus, B.E.; Bagley, M.B.; Ba- ñados, E.; et al. Broad-Line AGN at 3.5 < z < 6: The Black Hole Mass Function and a Connection with Little Red Dots . arXiv 2024, arXiv: 2409.06772...

  156. [164]

    Wang, B.; et al

    Greene, J.E.; Labbé, I.; Goulding, A.D.; Furtak, L.J.; Chemerynska, I.; Kokorev, V.; Dayal, P.; Volonteri, M.; Williams, C.C. ; Wang, B.; et al. UNCOVER Spectroscopy Confirms the Surprising Ubiquity of Active Galactic Nuclei in Red Sources at z > 5. Astrophys. J. 2024, 964, 39...

  157. [165]

    UNCOVER: Candidate Red Active Galactic Nuclei at 3<z<7 with JWST and ALMA

    Labbe, I.; Greene, J.E.; Bezanson, R.; Fujimoto, S.; Furtak, L.J.; Goulding, A.D.; Matthee, J.; Naidu, R.P.; Oesch, P.A.; Atek, H.; et al . UNCOVER: Candidate Red Active Galactic Nuclei at 3<z<7 with JWST and ALMA . arXiv 2023, arXiv :2306.07320. https://doi.org/10.48550/arXiv...

  158. [166]

    little red dots

    Akins, H.B.; Casey, C.M.; Lambrides, E.; Allen, N.; Andika, I.T.; Brinch, M.; Champagne, J.B.; Cooper, O.; Ding, X.; Drakos, N.E.; et al. COSMOS -Web: The over -abundance and physical nature of “little red dots ”--Implications for early galaxy and SMBH assembly. arXiv 2024, ar...

  159. [167]

    Silencing the Giant: Evidence of Active Galactic Nucleus Feedback and Quenching in a Little Red Dot at z = 4.13

    Kokorev, V.; Chisholm, J.; Endsley, R.; Finkelstein, S.L.; Greene, J.E.; Akins, H.B.; Bromm, V.; Casey, C.M.; Fujimoto, S.; Labbé, I.; et al. Silencing the Giant: Evidence of Active Galactic Nucleus Feedback and Quenching in a Little Red Dot at z = 4.13 . As- trophys. J. 2024,...

  160. [168]

    B., Casey, C

    Akins, H. B., Casey, C. M., Allen, N., Bagley, M. B., Dickinson, M., Finkelstein, S. L., Franco, M., Harish, S., Haro, P. A., Ilbert, et al. Two Massive, Compact, and Dust-obscured Candidate z 8 Galaxies Discovered by JWST. Astrophys. J. 2023, 956, 61

  161. [169]

    arXiv 2025, arXiv:2508.00057

    Tanaka, T.S.; Akins, H.B.; Har ikane, Y.; Silverman, J.D.; Casey, C.M.; et al.; Discovery of a Little Red Dot candidate at 𝑧 > 10 in COSMOS-Web based on MIRI-NIRCam selection. arXiv 2025, arXiv:2508.00057

  162. [170]

    Discovery of a n ew N-emitter in the epoch of reionization

    Schaerer, D.; Marques-Chaves, R.; Xiao, M.; Korber, D. Discovery of a n ew N-emitter in the epoch of reionization. Astron. As- trophys. 2024, 687, L11

  163. [171]

    A.; D’Eugenio, F.; Curti, M.; de Graaff, A.; Ji, Z.; Maiolino, R.; et al

    Baker, W.M.; Tacchella, S.; Johnson, B.D.; Nelson, E.; Suess, K. A.; D’Eugenio, F.; Curti, M.; de Graaff, A.; Ji, Z.; Maiolino, R.; et al. A core in a star -forming disc as evidence of inside -out growth in the early Universe . NatAs, 2024, Advanced Online Publica- tion

  164. [172]

    Efficient formation of a massive quiescent galaxy at redshift 4.9

    de Graaff, A.; Setton, D.J.; Brammer, G.; Cutler, S.; Suess, K.A.; Labbe, I.; Leja, J.; Weibel, A.; Maseda, M.V.; Whitaker, K.E.; et al. Efficient formation of a massive quiescent galaxy at redshift 4.9. arXiv 2024, arXiv:2404.05683

  165. [173]

    T.; et al

    Carnall, A.C.; McLure, R.J.; Dunlop, J.S.; McLeod, D.J.; Wild, V.; Cullen, F.; Magee, D.; Begley, R.; Cimatti, A.; Donnan, C. T.; et al. A massive quiescent galaxy at redshift 4.658. Nature 2023, 619, 716

  166. [174]

    Astrophys

    Setton, D.J.; Khullar, G.; Miller, T.B.; Bezanson, R.; Greene, J.E.; Suess, K.A.; Whitaker, K.E.; Antwi-Danso, J.; Atek, H.; Bram- mer, G.; et al UNCOVER NIRSpec/PRISM Spectroscopy Unveils Evidence of Early Core Formation in a Massive, Centrally Dusty Quiescent Galaxy at zspec...

  167. [175]

    JADES: Rest-frame UV-to-NIR Size Evolution of Massive Quiescent Galaxies from Redshift z=5 to z=0.5

    Ji, Z.; Williams, C.C.; Suess, K.A.; Tacchella, S.; Johnson, B.D.; Robertson, B.; Alberts, S.; Baker, W.M.; Baum, S.; Bhatawd ekar, R.; et al . JADES: Rest-frame UV-to-NIR Size Evolution of Massive Quiescent Galaxies from Redshift z=5 to z=0.5. arXiv 2024, arXiv:2401.00934

  168. [176]

    A high black hole to host mass ratio in a lensed AGN in the early Universe

    Furtak, L.J.; Labbé, I.; Zitrin, A.; Greene, J.E.; Dayal, P.; Chemerynska, I.; Kokorev, V.; Miller, T.B.; Goulding, A.D.; de Graaff, A.; et al. A high black hole to host mass ratio in a lensed AGN in the early Universe. Nature 2024, 628, 57–61

  169. [177]

    Remarkably Compact Quiescent Candidates at 3 < z < 5 in JWST-CEERS

    Wright, L.; Whitaker, K.E.; Weaver, J.R.; Cutler, A.M.; Wang, B.; Carnall, A.; Suess, K.A.; Bezanson, R.; Nelson, E.; Miller, T.B.; et al. Remarkably Compact Quiescent Candidates at 3 < z < 5 in JWST-CEERS. Astrophys. J. Lett. 2024, 964, L10. 22 of 22

  170. [178]

    JWST/NIRCam Probes Young Star Clusters in the Reionization Era Sunrise Arc

    Vanzella, E.; Claeyssens, A.; Welch, B.; Adamo, A.; Coe, D.; Diego, J.M.; Mahler, G.; Khullar, G.; Kokorev, V.; Oguri, M.; et al. JWST/NIRCam Probes Young Star Clusters in the Reionization Era Sunrise Arc. Astrophys. J. 2023, 945, 53

  171. [179]

    -H.; Malkan, M.A

    Bennert, V.N.; Auger, M.W.; Treu, T.; Woo, J. -H.; Malkan, M.A. The Relation between Black Hole Mass and Host Spheroid Stellar Mass Out to z ~ 2. Astrophys. J. 2011, 742, 107

  172. [180]

    JWST CEERS and JADES Active Galaxies at z = 4 –7 Violate the Local M•–M* Relation at >3σ: Implications for Low-mass Black Holes and Seeding Models

    Pacucci, F.; Nguyen, B.; Carniani, S.; Maiolino, R.; and Fan, X. JWST CEERS and JADES Active Galaxies at z = 4 –7 Violate the Local M•–M* Relation at >3σ: Implications for Low-mass Black Holes and Seeding Models. Astrophys. J. Lett. 2023, 957, L3

  173. [181]

    Maiolino, R.; Scholtz, J.; Curtis-Lake, E.; Carniani, S.; Baker, W.; de Graaff, A.; Tacchella, S.; Übler, H.; D’Eugenio, F.; Witstok, J.; et al. JADES. The diverse population of infant Black Holes at 4 < z < 11: Merging, tiny, poor, but mighty . arXiv 2023, arXiv:2308.01230

  174. [182]

    Sizes and Stellar Masses of the Little Red Dots Imply Immense Stellar Densities

    Guia, C.A.; Pacucci, F.; Kocevski, D.D. Sizes and Stellar Masses of the Little Red Dots Imply Immense Stellar Densities. Res. Notes AAS 2024, 8, 207

  175. [183]

    Exploring the AGN Fraction of a Sample of JWST’s Little Red Dots at 5 > z > 8 : Over- massive Black Holes Are Strongly Favored

    Durodola, E.; Pacucci, F.; Hickox, R.C. Exploring the AGN Fraction of a Sample of JWST’s Little Red Dots at 5 > z > 8 : Over- massive Black Holes Are Strongly Favored. arXiv 2024, arXiv:2406.10329

  176. [184]

    Supermassive Stars Match the Spectral Signatures of JWST's Little Red Dots

    Nandal, D.; Loeb, A. Supermassive Stars Match the Spectral Signatures of JWST's Little Red Dots . arXiv 2025, arXiv:2507.12618

  177. [185]

    What Is the Nature of Little Red Dots and what Is Not, MIRI SMILES Edition

    Pérez-González, P.G.; Barro, G.; Rieke, G.H.; Lyu, J.; Rieke, M.; Alberts, S.; Williams, C.C.; Hainline, K.; Sun, F.; Puskás, D.; et al. What Is the Nature of Little Red Dots and what Is Not, MIRI SMILES Edition. Astrophys. J. 2024, 968, 4

  178. [186]

    Structure and Evolution of the Stars; Dover: New York, NY, USA, 1958

    Schwarzschild, M. Structure and Evolution of the Stars; Dover: New York, NY, USA, 1958

  179. [187]

    The Discovery of Little Red Dots in the Local Universe: Signatures of Cool Gas Envelopes

    Lin, X.; Fan, X.; Cai, Z.; Bian, F.; Liu, H.; Sun, F.; Ma, Y.; Greene, J.E.; Strauss, M.A.; Green, R.; et al. The Discovery of Little Red Dots in the Local Universe: Signatures of Cool Gas Envelopes. arXiv 2025, arXiv:2507.10659

  180. [188]

    Ages of Stars

    Soderblom, D.R. Ages of Stars. Ann. Rev. Astron. Astrophys 2010, 48, 581

  181. [189]

    Stellar Structure and Evolution; Springer-Verlag: Heidelberg, Germany, 1990

    Kippenhahn, R.; Weigert, A. Stellar Structure and Evolution; Springer-Verlag: Heidelberg, Germany, 1990

  182. [190]

    How accurate are stellar ages based on stellar models? I

    Lebreton, Y.; Goupil, M.J.; Montalban, J. How accurate are stellar ages based on stellar models? I. The impact of stellar models uncertainties. EAS Publ. Ser. 2014, 65, 99–176

  183. [191]

    Ages of Stars: Methods and Uncertainties

    Soderblom, D.R. Ages of Stars: Methods and Uncertainties. arXiv 2014, arXiv:1409.2266

  184. [192]

    The age of the Methuselah star in the light of stellar evolution models with tailored abundances

    Guillaume, C.; Buldgen, G.; Amarsi, A.M.; Dupret, M.A.; Lundkvist, M.S.; Larsen, J.R.; Scuflaire, R.; Noels, A. The age of the Methuselah star in the light of stellar evolution models with tailored abundances. Astron. Astrophys. 2024, 692, L3

  185. [193]

    HD 140283: A Star in the S olar Neighborhood that Formed Shortly after the Big Bang

    Bond, H.E.; Nelan, E.P.; VandenBerg, D.A.; Schaefer, G.H.; Harmer, D. HD 140283: A Star in the S olar Neighborhood that Formed Shortly after the Big Bang. Astrophys. J. Lett. 2013, 765, L12

  186. [194]

    An unambiguous AGN and a Balmer break in an Ultraluminous Little Red Dot at z=4.47 from Ultradeep UNCOVER and All the Little Things Spectroscopy

    Labbé, I.; Greene, J.E.; Matthee, J.; Treiber, H.; Kokorev, V.; Miller, T.B.; Kramarenko, I.; Setton, D.J.; Ma, Y.; Goulding, A.D.; et al. An unambiguous AGN and a Balmer break in an Ultraluminous Little Red Dot at z=4.47 from Ultradeep UNCOVER and All the Little Things Spectr...

  187. [195]

    Could the number of blue straggler stars help to determine the age of their parent globular cluster? arXiv 2023, arXiv: 2308.09057

    de Andrés, F.L. Could the number of blue straggler stars help to determine the age of their parent globular cluster? arXiv 2023, arXiv: 2308.09057

  188. [196]

    Galaxy build -up in the first 1.5 Gyr of cosmic history: Insights from the stellar mass function at z ~ 4 –9 from JWST NIRCam observations

    Weibel, A.; Oesch, P.A.; Barrufet, L.; Gottumukkala, R.; Ellis, R.S.; Santini, P.; Weaver, J.R.; Allen, N .; Bouwens, R.; Bowler, R.A.A.; et al. Galaxy build -up in the first 1.5 Gyr of cosmic history: Insights from the stellar mass function at z ~ 4 –9 from JWST NIRCam observ...

  189. [197]

    Where Stars Form: Inside-out Growth and Coherent Star Formation from HST Hα Maps of 3200 Galaxies across the Main Sequence at 0.7 < z < 1.5

    Nelson, E.J.; van Dokkum, P.G.; Schreiber, N.M.F.; Franx, M.; Brammer, G.B.; Momcheva, I.G.; Wuyts, S.; Whitaker, K.E.; Skelton, R.E.; Fumagalli, M.; et al. Where Stars Form: Inside-out Growth and Coherent Star Formation from HST Hα Maps of 3200 Galaxies across the Main Sequen...

  190. [199]

    Williams, C.C.; Oesch, P.A.; Elbaz, D.; Dessauges-Zavadsky, M.; Marques-Chaves, R.; Bing, L.; Ji, Z.; Weibel, A.; Bezanson, R.; et al

    Xiao, M. ; Williams, C.C.; Oesch, P.A.; Elbaz, D.; Dessauges-Zavadsky, M.; Marques-Chaves, R.; Bing, L.; Ji, Z.; Weibel, A.; Bezanson, R.; et al. PANORAMIC: Discovery of an ultra-massive grand-design spiral galaxy at z ~ 5.2. Astron. Astrophys. 2025, 696, A156

  191. [6110]

    https://doi.org/10.1093/mnras/stad3597

Pith tools

Reviewed August 4, 2026 · model on record in the stance chip above.