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arxiv: 2606.11328 · v1 · pith:WR6C26WEnew · submitted 2026-06-09 · 🌌 astro-ph.GA

Morphology, sizes, and scatter in a large sample of distant quiescent galaxies

G. Scarpe , F. Valentino , K. Ito , M. W. Baker , A. Pensabene , P. Zhu This is my paper

Pith reviewed 2026-06-27 12:21 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords quiescent galaxiesgalaxy sizesstellar mass-size relationhigh-redshift galaxiesSersic profilesJWSTgalaxy morphologyquenching
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The pith

Stellar mass and redshift suffice to predict sizes of quiescent galaxies at z>3, with large remaining scatter.

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

The study assembles a sample of 137 massive quiescent galaxy candidates at redshifts 3 to 7 across JWST fields and models their surface brightness with Sersic profiles in five bands. Sizes decrease with redshift and with observed wavelength, the latter effect being stronger at lower stellar mass, while the scatter around the mass-size relation shows no dependence on redshift or band. A Bayesian analysis testing multiple parameters finds that axis ratio, Sersic index, UVJ colors, and environment add no significant predictive power beyond stellar mass and redshift. This leaves a large intrinsic scatter that standard Sersic descriptors cannot account for, indicating other physical quantities are needed to trace post-quenching growth paths.

Core claim

In 137 quiescent candidates at 3<z<7, the size-mass relation is consistent with prior results and extends to z_spec=4.9, with size decreasing at higher redshift. Intrinsic scatter is independent of redshift and filter. Size decreases with wavelength, with the gradient decreasing at higher stellar mass, while Sersic index is wavelength-independent. Forward and backward Bayesian fits show no significant secondary dependence on axis ratio q, Sersic index n, UVJ-colors, or environment, so stellar mass and redshift alone predict size, albeit with large scatter that requires other physical quantities.

What carries the argument

Forward and backward Bayesian fitting applied to the stellar mass-size relation derived from multi-band Sersic modeling to test for secondary parameter dependencies.

If this is right

  • Size decreases with increasing redshift, extending prior trends to z_spec=4.9.
  • Size decreases with increasing observed wavelength, with a steeper gradient at lower stellar mass.
  • Sersic index shows no significant dependence on wavelength, independent of stellar mass.
  • No significant secondary dependence of size on axis ratio, Sersic index, UVJ-colors, or environment.
  • Stellar mass and redshift together predict size, but large intrinsic scatter remains unexplained by Sersic parameters.

Where Pith is reading between the lines

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

  • Merger histories or variations in dark matter halo assembly could be among the additional factors needed to explain the scatter.
  • Spectroscopic follow-up on a subset would directly test selection purity and its impact on the measured scatter.
  • The wavelength dependence of size points to radial stellar population gradients that may distinguish growth modes.
  • Repeating the Bayesian test on lower-mass or higher-redshift samples could show when mass and redshift become dominant predictors.

Load-bearing premise

The 137 objects selected by photometric criteria are genuine quiescent galaxies with minimal contamination from dusty star-forming systems.

What would settle it

Spectroscopic confirmation that a substantial fraction of the photometrically selected sample are actually star-forming galaxies would change the reported size trends and scatter values.

Figures

Figures reproduced from arXiv: 2606.11328 by A. Pensabene, F. Valentino, G. Scarpe, K. Ito, M. W. Baker, P. Zhu.

Figure 1
Figure 1. Figure 1: UV J diagram of the final vetted sample after visual inspection, color coded by redshift. The black lines show the selection box in Williams et al. (2009), extended at the blue end to include recently quenched systems (Schreiber et al. 2018; Belli et al. 2019) [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Wavelength gradients of the effective size and Sérsic index as a function of the stellar mass. Our sample is indicated by filled circles, color-coded by redshift. The uncertainty on the stellar mass is fixed at 0.21 dex. The median value of the sample is marked by the red filled square, while the pink triangle shows the result in Ito et al. 2024. The black solid line and blue shaded area indicate the best-… view at source ↗
Figure 3
Figure 3. Figure 3: Stellar mass–size relation for quiescent systems at [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Median size evolution for a M⋆ = 5 × 1010 M⊙ quies￾cent galaxy with redshift. The red and blue symbols indicate our median measurements in the F200W and F444W filters, respec￾tively; squares show the median of the sample in the z = 3 − 5 range, while diamonds show binned samples. Pink square and circles show the equivalent medians from Ito et al. (2024). The black circles indicate the measurements in van d… view at source ↗
Figure 5
Figure 5. Figure 5: Bulge-to-total ratio as a function of Sérsic indices from a simple Sérsic profile (in the F444W, top-left, and F200W bands, [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: In the upper-right panel we indicate with [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
read the original abstract

After quenching galaxies keep growing in size across time, as established in the literature up to cosmic noon. In this work, we assemble one of the largest and most comprehensive multi-wavelength photometric sample of massive quenched galaxies at z > 3, counting 137 quiescent candidates within 825 sq.arcmin and redshift 3<z<7 across the well-studied extragalactic JWST fields. We model their surface brightness distribution across 5 bands mapping their UV-to-NIR rest-frame wavelength with Sersic profiles, and derive their sizes, concentrations, and ellipticities. The size-mass relation is consistent with previous studies. Size decreases with increasing redshift, in agreement with previous studies and extending them up to z_spec=4.9. The intrinsic scatter of the mass-size relation has no relevant dependence on the redshift and the filter used. Our multi-wavelength modeling reveals that size decreases with increasing observed wavelength, and the wavelength gradient decreases with increasing stellar mass. This result proves that in the NIR-bands massive elliptical galaxies appear more compact. The Sersic index does not show significant dependence on wavelength, independently of the stellar mass. Following a forward/backward Bayesian fit analysis to assess the significance of several parameters in predicting the size of our sample, we do not identify any significant secondary dependence of the size on axis ratio q, Sersic index n, UVJ-colors, and environment. The combination of stellar mass and redshift is sufficient to predict the size of quiescent galaxies at z>3, albeit with a large scatter. This suggests that the commonly used parameters of a Sersic distribution cannot explain the large intrinsic scatter around the stellar mass-size relation, suggesting that other physical quantities need to be taken into account to break the degeneracy between evolution paths across the galaxy population.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The paper assembles one of the largest photometric samples of 137 quiescent galaxy candidates at 3<z<7 across JWST fields, fits multi-band Sersic profiles to derive sizes, concentrations and ellipticities, and reports that the size-mass relation is consistent with prior work, that sizes decrease with redshift and observed wavelength (with the gradient weakening at higher mass), and that a Bayesian forward/backward selection finds stellar mass plus redshift sufficient to predict size with no significant secondary dependence on Sersic index n, axis ratio q, UVJ colors or environment. The large intrinsic scatter around the relation is independent of redshift and filter and is not explained by standard Sersic parameters.

Significance. If the photometric quiescent selection is robust and the size measurements are unbiased, the work extends the mass-size relation and its scatter properties to z~5 with a statistically useful sample size, and the finding that commonly used Sersic parameters do not account for the scatter would motivate searches for additional physical drivers of size evolution at early times.

major comments (2)
  1. [Sample selection] Sample selection (abstract and §2): the central claim that mass + redshift suffice and that no secondary parameters matter rests on the 137 objects being genuine quiescent systems. At z>3 photometric UVJ or similar cuts are known to admit non-negligible contamination from dusty star-formers whose sizes and colors differ systematically; any impurity directly biases the reported intrinsic scatter, wavelength dependence, and the Bayesian predictor selection. A quantitative purity assessment or spectroscopic validation fraction is required.
  2. [Bayesian analysis] Bayesian forward/backward fit (abstract): the statement that n, q, UVJ and environment show “no significant secondary dependence” requires explicit reporting of the model evidence ratios, prior choices, and how the large intrinsic scatter is propagated into the significance thresholds; without these the conclusion that mass + redshift are sufficient cannot be evaluated.
minor comments (2)
  1. [Abstract] The abstract states “the intrinsic scatter … has no relevant dependence on the redshift and the filter used” but does not quote the measured scatter values or their uncertainties; these should be tabulated.
  2. [Methods] Clarify the exact wavelength range and filter set used for the five-band modeling and whether the reported size-wavelength trend is measured at fixed rest-frame or observed-frame wavelengths.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive comments. We address the two major points below and will revise the manuscript to strengthen the presentation of sample purity and the Bayesian analysis details.

read point-by-point responses

  1. Referee: [Sample selection] Sample selection (abstract and §2): the central claim that mass + redshift suffice and that no secondary parameters matter rests on the 137 objects being genuine quiescent systems. At z>3 photometric UVJ or similar cuts are known to admit non-negligible contamination from dusty star-formers whose sizes and colors differ systematically; any impurity directly biases the reported intrinsic scatter, wavelength dependence, and the Bayesian predictor selection. A quantitative purity assessment or spectroscopic validation fraction is required.

    Authors: We agree that quantitative assessment of photometric selection purity is important at z>3. Our UVJ selection follows standard criteria from the literature, but to address this we will add a new paragraph in §2 that provides a quantitative estimate of expected contamination from dusty star-formers, based on recent JWST-specific simulations and studies. We will also report the spectroscopic validation fraction for the subset of sources with available spec-z confirming quiescence. These changes will be incorporated in the revised version. revision: yes

  2. Referee: [Bayesian analysis] Bayesian forward/backward fit (abstract): the statement that n, q, UVJ and environment show “no significant secondary dependence” requires explicit reporting of the model evidence ratios, prior choices, and how the large intrinsic scatter is propagated into the significance thresholds; without these the conclusion that mass + redshift are sufficient cannot be evaluated.

    Authors: We appreciate the request for additional methodological transparency. In the revised manuscript we will expand the description of the forward/backward Bayesian analysis (in the methods section and/or an appendix) to include the specific prior choices, the computed model evidence ratios (or Bayes factors) for models including versus excluding secondary parameters, and an explicit statement of how the intrinsic scatter enters the significance assessment. This will allow full evaluation of the claim that stellar mass plus redshift suffice. revision: yes

Circularity Check

0 steps flagged

No circularity: purely empirical observational analysis

full rationale

The paper assembles a photometric sample of 137 z>3 quiescent candidates, fits Sersic profiles across bands to extract sizes/n/q, and applies forward/backward Bayesian regression to test secondary predictors of size. All reported relations (size-mass, size-redshift, wavelength dependence, lack of secondary dependence on n/q/UVJ/environment) are direct statistical outputs from the data and standard modeling; none reduce by the paper's own equations to a fitted parameter renamed as prediction, a self-citation chain, or a self-definitional loop. The central claim that mass+redshift suffice is an empirical finding from the regression, not a tautology. No load-bearing self-citations or imported uniqueness theorems appear in the provided text.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

Abstract-only review supplies almost no explicit free parameters, axioms, or invented entities; the analysis rests on standard assumptions of Sersic morphology and photometric quiescence selection that are not quantified here.

axioms (2)
  • domain assumption Sersic profiles provide an adequate description of the surface-brightness distribution of high-redshift quiescent galaxies across UV-to-NIR rest-frame wavelengths
    Invoked implicitly by the modeling step described in the abstract.
  • domain assumption Photometric criteria reliably isolate quiescent galaxies with low contamination at 3<z<7
    Required for the sample of 137 candidates to represent the intended population.

pith-pipeline@v0.9.1-grok · 5876 in / 1410 out tokens · 20846 ms · 2026-06-27T12:21:07.761645+00:00 · methodology

discussion (0)

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Reference graph

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