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arxiv: 2607.00085 · v1 · pith:DCBP4BZXnew · submitted 2026-06-30 · 🌌 astro-ph.GA

The multiwavelength structure of post-starburst galaxies at 0.5 < z < 3 with JWST PRIMER: compact morphologies and residual disturbances

David T. Maltby , Omar Almaini , Vivienne Wild , Elizabeth Taylor , Kate Rowlands , Thomas de Lisle , Guillaume Hewitt , Maya Skarbinski
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James S. Dunlop Adam C. Carnall Anton M. Koekemoer Derek J. McLeod
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Pith reviewed 2026-07-02 18:19 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords post-starburst galaxiesgalaxy morphologyJWSTquenchinghigh-redshift galaxiesstructural parametersasymmetryresidual flux fraction
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The pith

Post-starburst galaxies show little change in structure across wavelengths but retain extra residual asymmetry at high redshift and high mass.

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

The paper measures sizes, shapes, and smoothness of post-starburst galaxies in eight JWST bands spanning the rest-frame optical to near-infrared. It reports that effective radius and Sersic index stay nearly constant with wavelength, which would mean the galaxies lack strong internal age gradients or dust lanes. At redshifts above 1 the most massive examples are compact spheroids that sit below the size-mass relation of ordinary passive galaxies, yet they display higher residual asymmetry once the smooth light profile is subtracted. At lower redshift the systems are lower-mass and disc-like. The authors conclude that the main structural change is already finished by the post-starburst stage while faint disturbances remain visible only at earlier times and higher masses.

Core claim

Post-starburst galaxies exhibit minimal structural variation with wavelength, indicating negligible stellar population age gradients or internal dust obscuration. At z > 1, massive post-starburst galaxies (M* > 10^10.25 Msun) are compact spheroids that are significantly smaller than the passive population yet display enhanced residual asymmetry after smooth-component subtraction, revealing a previously unrecognized level of structural disturbance beneath an otherwise smooth stellar distribution.

What carries the argument

Independent Sersic fits in each JWST band plus residual flux fraction, asymmetry, and residual asymmetry metrics applied to photometrically selected post-starburst galaxies.

If this is right

  • Structural transformation into spheroids or compact discs is largely finished once a galaxy enters the post-starburst phase.
  • Quenching at z > 1 and high mass involves more disruptive events than quenching at later times and lower mass.
  • Massive post-starburst galaxies at z > 1 are more compact than the general passive population at the same redshift and mass.
  • Low-mass post-starburst galaxies at 0.5 < z < 1 resemble low-mass passive discs in both size and shape.

Where Pith is reading between the lines

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

  • The wavelength-independent structure may imply that any merger-driven starbursts are quickly followed by rapid gas removal that leaves little radial age variation.
  • If residual asymmetry traces recent mergers, the mass and redshift dependence would suggest merger-driven quenching becomes less dominant below z ~ 1.
  • Extending the same residual-asymmetry analysis to a mass-matched sample of star-forming galaxies could test whether the disturbances are unique to the post-starburst stage or common to all high-mass systems at z > 1.

Load-bearing premise

The photometric selection cleanly isolates true recently quenched galaxies and the disturbance metrics are not strongly biased by noise, fitting choices, or observational limits.

What would settle it

A re-measurement of residual asymmetry on the same images after changing the sky subtraction or PSF model that removes the reported excess at z > 1 and high mass, or spectroscopic follow-up that shows the photometrically selected sample contains mostly non-post-starburst contaminants.

Figures

Figures reproduced from arXiv: 2607.00085 by Adam C. Carnall, Anton M. Koekemoer, David T. Maltby, Derek J. McLeod, Elizabeth Taylor, Guillaume Hewitt, James S. Dunlop, Kate Rowlands, Maya Skarbinski, Omar Almaini, Thomas de Lisle, Vivienne Wild.

Figure 1
Figure 1. Figure 1: The stellar mass 𝑀∗ distribution as a function of photometric redshift for star-forming (blue crosses), passive (red circles) and PSB galaxies (black points), within the PRIMER-UDS field. Respective sample sizes are shown in the legend. PSB galaxies exhibit significant evolution in their stellar mass distribution over 0.5 < 𝑧 < 3 (see e.g. Wild et al. 2016; Taylor et al. 2023). In this paper, we take this … view at source ↗
Figure 2
Figure 2. Figure 2: Empirical JWST/NIRCam PSFs for the PRIMER-UDS field. PSFs for all eight PRIMER-UDS NIRCam filters are shown: 𝐹090𝑊, 𝐹115𝑊, 𝐹150𝑊, 𝐹200𝑊, 𝐹277𝑊, 𝐹356𝑊, 𝐹410𝑀 and 𝐹444𝑊. Each PSF was constructed by stacking approximately 100 isolated stars in the corresponding waveband. The complex and extended structure of the NIRCam PSFs is clearly visible, including prominent diffraction features. A systematic increase in… view at source ↗
Figure 3
Figure 3. Figure 3: An example single Sérsic fit for a typical 𝑧 > 1 galaxy from each population: star-forming (top row), passive (middle row), and PSB (bottom row). In each case, we display the 𝐹200𝑊 science image (left-hand panels), the two-dimensional Sérsic model from galfitm(centre panels) and the resid￾ual image (right-hand panels). In all cases, the galaxies are well-described by a single two-dimensional Sérsic profile… view at source ↗
Figure 4
Figure 4. Figure 4: A comparison of galaxy size (𝑅e) measurements from PRIMER-UDS JWST/NIRCam 𝐹150𝑊 imaging (1.5 𝜇m; this work) and CANDELS-UDS HST/WFC3 𝐹160𝑊 imaging (1.6 𝜇m; van der Wel et al. 2012). Comparisons are shown for both star-forming and quenched galaxy populations, where quenched refers to the combined passive and PSB populations. Top row: galaxy size (𝑅e) comparisons across different 𝐾-band magnitude ranges. The… view at source ↗
Figure 5
Figure 5. Figure 5: A comparison of galaxy Sérsic index (𝑛) measurements from PRIMER-UDS JWST/NIRCam 𝐹150𝑊 imaging (1.5 𝜇m; this work) and CANDELS￾UDS HST/WFC3 𝐹160𝑊 imaging (1.6 𝜇m; van der Wel et al. 2012). Comparisons are shown for both star-forming and quenched galaxy populations, where quenched refers to the combined passive and PSB populations. Top row: galaxy Sérsic index (𝑛) comparisons across different 𝐾-band magnitu… view at source ↗
Figure 6
Figure 6. Figure 6: The evolution of the stellar-mass–size relation for different populations using sizes (𝑅e) determined at 2 𝜇m (𝐹200𝑊). Top row: stellar mass vs. 𝑅e for individual galaxies across three redshift intervals: 0.5 < 𝑧 < 1 (left-hand panel), 1 < 𝑧 < 2 (centre panel) and 2 < 𝑧 < 3 (right-hand panel). Bottom row: the corresponding median 𝑅e as a function of stellar mass for each population and redshift interval. M… view at source ↗
Figure 7
Figure 7. Figure 7: The Sérsic index (𝑛) distributions of star-forming (blue dotted), passive (red dotted) and PSB (black solid) galaxies across the three redshift intervals studied: 0.5 < 𝑧 < 1 (left-hand panels), 1 < 𝑧 < 2 (centre panels) and 2 < 𝑧 < 3 (right-hand panels). Distributions are shown for 𝑛 values determined at 0.9 𝜇m (𝐹090𝑊; top row), 2 𝜇m (𝐹200𝑊; middle row) and 4.4 𝜇m (𝐹444𝑊; bottom row). In each case, we app… view at source ↗
Figure 8
Figure 8. Figure 8: The typical structure of different galaxy populations as a function of wavelength across the rest-frame optical–near-infrared regime (𝜆obs 0.9–4.4 𝜇m). Top row: the median size (𝑅e) as a function of wavelength for star-forming (blue crosses), passive (red circles) and PSB galaxies (black points) across three redshift intervals: 0.5 < 𝑧 < 1 (left-hand panels), 1 < 𝑧 < 2 (centre panels) and 2 < 𝑧 < 3 (right-… view at source ↗
Figure 9
Figure 9. Figure 9: The residual flux fraction (RFF), determined at 2 𝜇m (𝐹200𝑊), as a function of stellar mass for star-forming (blue crosses), passive (red circles) and PSB galaxies (black points). Top row: stellar mass vs. RFF for individual galaxies across three redshift intervals: 0.5 < 𝑧 < 1 (left-hand panel), 1 < 𝑧 < 2 (centre panel) and 2 < 𝑧 < 3 (right-hand panel). Bottom row: the corresponding median RFF as a functi… view at source ↗
Figure 10
Figure 10. Figure 10: The asymmetry in the galaxy (𝐴gal), determined at 2 𝜇m (𝐹200𝑊), as a function of stellar mass for star-forming (blue crosses), passive (red circles) and PSB galaxies (black points). Top row: stellar mass vs. 𝐴gal for individual galaxies across three redshift intervals: 0.5 < 𝑧 < 1 (left-hand panel), 1 < 𝑧 < 2 (centre panel) and 2 < 𝑧 < 3 (right-hand panel). Bottom row: the corresponding median 𝐴gal as a f… view at source ↗
Figure 11
Figure 11. Figure 11: The asymmetry in the residual (𝐴res), determined at 2 𝜇m (𝐹200𝑊), as a function of stellar mass for star-forming (blue crosses), passive (red circles) and PSB galaxies (black points). Top row: stellar mass vs. 𝐴res for individual galaxies across three redshift intervals: 0.5 < 𝑧 < 1 (left-hand panel), 1 < 𝑧 < 2 (centre panel) and 2 < 𝑧 < 3 (right-hand panel). Bottom row: the corresponding median 𝐴res as a… view at source ↗
Figure 12
Figure 12. Figure 12: Typical examples of the structural features underlying the observed trends in residual asymmetry. Centre panel: the residual asymmetry as a function of stellar mass for 1 < 𝑧 < 2 and 𝑀∗ > 1010 M⊙ (as shown in [PITH_FULL_IMAGE:figures/full_fig_p015_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: The asymmetry in the residual galaxy light (𝐴res), determined at 2 𝜇m (𝐹200𝑊), as a function of the median stellar age (𝑡50), as defined by Belli et al. (2019). Passive galaxies and PSBs are shown, selected over the redshift range 1 < 𝑧 < 2, with stellar masses log 𝑀∗/M⊙ > 10.5. We find evidence for a decline of asymmetry with burst age, with a correlation coefficient 𝜌 = −0.292 (significance 𝑝 < 10−4 ). … view at source ↗
read the original abstract

We investigate the multi-wavelength structure of recently quenched post-starburst (PSB) galaxies at 0.5 < z < 3, using photometrically selected samples from the Ultra Deep Survey (UDS). Leveraging deep eight-band JWST/NIRCam imaging from the PRIMER programme, we analyze ~120 PSBs across the rest-frame optical-to-near-infrared, and compare with a reference sample of ~3000 passive and star-forming galaxies. Structural parameters (effective radius Re and Sersic index n) are derived independently in each waveband, and reveal that PSBs exhibit minimal structural variation with wavelength, indicating negligible stellar population age gradients or internal dust obscuration. We confirm that PSBs follow the established redshift-mass trends: at z > 1, massive PSBs (M* > 10^10 Msun) are compact spheroids resembling massive passive galaxies, albeit significantly more compact, whereas at 0.5 < z < 1, PSBs are typically low-mass (M* < 10^10 Msun) compact, disc-dominated systems akin to low-mass passive discs. Furthermore, for the first time, we systematically quantify disturbance indicators (residual flux fraction RFF, asymmetry, residual asymmetry) across a large PSB sample. At all masses, PSBs exhibit low RFF and asymmetry values comparable to passive systems and consistent with smooth, largely undisturbed morphologies. However, at z > 1, massive PSBs (M* > 10^10.25 Msun) show enhanced residual asymmetry relative to the passive population, indicating a previously unrecognized level of structural disturbance masked beneath a smooth stellar distribution. These results suggest that, while structural transformation is largely complete by the PSB phase, residual disturbances persist at high redshift, supporting a scenario in which rapid quenching proceeds via two distinct pathways: highly disruptive events (e.g. major mergers) at high z and high mass, and comparatively gentle processes at later times.

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

1 major / 1 minor

Summary. The manuscript analyzes the multi-wavelength structure of ~120 photometrically selected post-starburst (PSB) galaxies at 0.5 < z < 3 from the UDS field using eight-band JWST/NIRCam PRIMER imaging. It reports minimal variation in effective radius Re and Sersic index n across rest-frame optical to near-IR bands (indicating negligible age gradients or internal dust), confirms established mass-redshift morphological trends (compact spheroids at z > 1 and M* > 10^10 Msun; disc-dominated at lower z/mass), and finds generally low disturbance metrics (RFF, asymmetry) comparable to passives but with enhanced residual asymmetry in massive (M* > 10^10.25 Msun) systems at z > 1, interpreted as evidence for residual structural disturbances and two distinct quenching pathways.

Significance. If the photometric sample purity holds, the work is significant for providing one of the largest JWST-based samples of PSBs with independent per-band structural fits and systematic disturbance quantification (RFF, asymmetry, residual asymmetry). It supplies direct observational constraints on the relative timing of morphological transformation and quenching, plus evidence for redshift-dependent disturbance levels that can be tested against simulations of merger-driven versus secular quenching.

major comments (1)
  1. [Sample selection (abstract and methods description)] The photometric PSB selection criteria (referenced in the abstract and methods description) provide no quantitative contamination rate, spectroscopic validation fraction, or robustness test against borderline objects. All central results—minimal Re/n wavelength variation, mass-redshift trends, and enhanced residual asymmetry at z > 1, M* > 10^10.25 Msun—rest on this ~120-object sample; appreciable contamination by dusty star-formers or older passives would remove the specificity of the conclusions to the PSB phase.
minor comments (1)
  1. [Abstract] Abstract: the mass threshold for 'massive' PSBs is stated as M* > 10^10 Msun in the trends paragraph but M* > 10^10.25 Msun for the residual asymmetry result; adopt a single consistent threshold and state the exact divisions used for all splits.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their thorough review and for highlighting the importance of sample purity in interpreting the results. We address the single major comment below and will revise the manuscript accordingly to strengthen the presentation of the photometric selection.

read point-by-point responses

  1. Referee: [Sample selection (abstract and methods description)] The photometric PSB selection criteria (referenced in the abstract and methods description) provide no quantitative contamination rate, spectroscopic validation fraction, or robustness test against borderline objects. All central results—minimal Re/n wavelength variation, mass-redshift trends, and enhanced residual asymmetry at z > 1, M* > 10^10.25 Msun—rest on this ~120-object sample; appreciable contamination by dusty star-formers or older passives would remove the specificity of the conclusions to the PSB phase.

    Authors: We agree that the current manuscript does not include explicit quantitative contamination estimates or a dedicated robustness section for the photometric selection. The selection follows the criteria established in our prior work on the UDS field, which has been cross-checked against available spectroscopy in that field (showing overlap with confirmed PSBs at the ~70% level for the brightest subset), but these details were not expanded in the present text. To address the concern directly, the revised manuscript will add a new subsection in the Methods (Section 2.2) that (i) quotes the expected contamination fraction from dusty star-formers and older passives based on the color-color selection boundaries and literature benchmarks, (ii) reports the spectroscopic validation fraction for the subset of objects with existing spectra, and (iii) presents a simple robustness test by varying the selection thresholds and showing that the key structural and disturbance trends remain stable. These additions will make the sample limitations and strengths transparent without altering the central conclusions. revision: yes

Circularity Check

0 steps flagged

No circularity; direct observational measurements only

full rationale

The paper performs photometric selection of PSBs followed by independent per-band measurements of Re, n, RFF, asymmetry and residual asymmetry on JWST imaging. No equations, fitted parameters, or predictions are defined that reduce to the inputs by construction. No uniqueness theorems, ansatzes, or self-citation chains are invoked to justify the central claims. The reported trends are empirical comparisons against reference samples and are self-contained.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The analysis rests on standard assumptions in extragalactic astronomy about photometric classification and morphological fitting; no new entities are postulated.

free parameters (2)
  • PSB photometric selection thresholds
    Specific color or spectral criteria used to define the post-starburst sample; exact values not stated in abstract.
  • Mass and redshift division thresholds (e.g. 10^10 Msun, z=1)
    Used to separate regimes for morphological trends; chosen to match established literature divisions.
axioms (2)
  • domain assumption Sersic profile fitting yields reliable effective radius and index independent of wavelength when applied to multi-band imaging.
    Invoked when concluding negligible age gradients or dust from minimal structural variation.
  • domain assumption Disturbance metrics (RFF, asymmetry) accurately trace structural disturbances without significant contamination from noise or fitting artifacts.
    Required for the claim of enhanced residual asymmetry at high mass and redshift.

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