Mass--size evolution and the emerging passive--density relation revealed by JWST/NIRCam in the Spiderweb protocluster

A. Naufal; B. Haussler; H. Dannerbauer; J. M. P\'erez-Mart\'inez; J. Nadolny; K. Daikuhara; M. Huertas-Company; P. G. P\'erez-Gonz\'alez; T. Kodama; Y. H. Zhang

REVIEW 2 major objections 6 minor 299 references

Mass--size evolution and the emerging passive--density relation revealed by JWST/NIRCam in the Spiderweb protocluster

T0 review · 2 major / 6 minor · reviewed 2026-07-14 · grok-4.5

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Pith's one-line read In the Spiderweb protocluster at z=2.16, quenching and structural change are already advanced while size growth is still ongoing.

desk verdict Solid JWST structural census of Spiderweb: intermediate passive MSR intercept and local-density-driven passive fraction, limited mainly by small passive N. read the letter →

arxiv 2607.11448 v1 pith:RXFUY2JQ submitted 2026-07-13 astro-ph.GA

J. Nadolny , J. M. Pérez-Martínez , H. Dannerbauer , B. Haussler , M. Huertas-Company , K. Daikuhara , T. Kodama , Y. Koyama

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A. Naufal P. G. Pérez-González Y. H. Zhang

This is my paper · ORCID

classification astro-ph.GA

keywords protoclustermass-sizerelationpassive-densityJWST/NIRCamgalaxystructureenvironmentalquenchingbulge-discdecompositionSpiderweb

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

This paper measures how environment shapes galaxy structure inside the Spiderweb protocluster at redshift 2.16, when clusters are still assembling. Using JWST/NIRCam imaging, the authors fit light profiles for 103 member galaxies and compare star-forming and passive systems to coeval field and cluster samples. Star-forming galaxies sit on a mass–size relation close to the field; passive galaxies show a flatter relation whose typical size lies between field and virialised-cluster values. The fraction of passive galaxies rises with local density from field-like levels to about 60 percent in the densest regions, with little extra dependence on distance from the cluster centre. The result paints the protocluster as a transitional environment: quenching and morphological change have already begun, yet size growth of the passive population is incomplete.

What carries the argument

Homogeneous multi-band single-Sérsic and bulge–disc parametric modelling of JWST/NIRCam F115W, F182M and F410M images for 103 protocluster members, combined with local density Σ3 (distance to the third nearest neighbour) and a star-formation main-sequence cut that defines the passive subsample.

What would settle it

A larger spectroscopic sample of Spiderweb members with uniform star-formation rates and rest-frame UVJ colours that reclassifies the same galaxies and re-fits the passive mass–size intercept; if that intercept moves fully onto the field or fully onto the virialised-cluster locus, the intermediate-stage claim fails.

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Extended reading notes

Core claim

Passive galaxies in the Spiderweb protocluster follow a flatter mass–size relation whose intercept (typical size at fixed stellar mass of 5 imes10^10 solar masses) lies between coeval field and cluster passive populations, while the passive fraction rises primarily with local projected density from field-like values to ~60 percent at the highest densities, indicating that quenching and structural transformation are already advanced while size growth is still ongoing.

Load-bearing premise

The claim rests on defining passive galaxies as those lying well below the star-formation main sequence, using only the modest number of objects that have measured star-formation rates, and treating that selection as comparable to colour-based passive samples used for the field and cluster comparisons.

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Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

The real news here is a homogeneous multi-band single-Sérsic plus bulge–disc analysis of 103 Spiderweb members with JWST/NIRCam, giving a passive mass–size intercept that sits between coeval field and cluster samples, plus a clear rise in passive fraction with local density Σ3 up to ~60% at the densest bins. That intermediate stage is the useful takeaway for quenching models.

What they do well is the uniform GALAPAGOS-2 multi-wavelength fitting, the wavelength trends (mild for the bulk sample, steep for the ALMA dusty systems), and the explicit robustness checks: z_spec-only, stricter 1-dex-below-SFMS cut, and a footprint-restricted density test. Slopes, intercepts, and the passive–density trend hold under those cuts. Bulges are systematically more compact than discs in both SFGs and passives, which is cleanly shown. Citations to van der Wel, Ward, Martorano, Shuntov, Mei, Afanasiev, and the prior Spiderweb HAE/ALMA papers are appropriate; no circularity.

Soft spots are real but already flagged by the authors. Only 14 galaxies have SFRs that put them below the Speagle SFMS (and only a handful have n>3), so the passive MSR intercept and the high-density passive-fraction bins carry large Wilson errors. The SFMS cut is not identical to the UVJ selections used in the comparison samples; they note Nedkova et al. found MSR intercepts largely insensitive to quiescence definition, and their own stricter cut does not change the result, but the comparison remains first-order. No correlation of size or ΣSFR with density is a null result, not a flaw. Methods are standard; nothing load-bearing is broken.

This is for people working on z~2 protoclusters, environmental quenching, and JWST structural scaling relations. It is a clear extension of the existing Spiderweb literature, not a reorganisation of the field. I would send it to referees; the data and checks are good enough that the small-N and selection caveats can be handled in revision. Worth citing for the intermediate intercept and the density-driven passive fraction once the catalogue is public.

Referee Report

2 major / 6 minor

Summary. The paper presents a homogeneous multi-band structural analysis of 103 Spiderweb protocluster members at z=2.16 using JWST/NIRCam F115W, F182M and F410M imaging. Single-Sérsic and bulge–disc fits with GALAPAGOS-2/GALFIT-M yield mass–size relations (MSRs) for star-forming and passive galaxies, wavelength-dependent sizes, and a passive-fraction versus local density (Σ3) relation. SFGs follow a field-like MSR (mildly steeper at high mass within uncertainties). Passive galaxies show a flatter MSR whose intercept at 5×10^10 M⊙ lies between coeval field and cluster passive populations. Bulges are more compact than discs; sizes decrease mildly with wavelength except for ALMA-detected dusty SFGs, which show a steep gradient. The passive fraction rises from field-like values at low Σ3 to ~60% at Σ ≳ 1000 gal Mpc^{-2}, with no strong additional dependence on clustercentric radius, and a weak density–Sérsic-index correlation (strongest in F410M). The authors interpret this as advanced quenching and structural transformation with size growth still ongoing.

Significance. If the intermediate passive MSR intercept and the local-density-driven passive fraction hold, the work supplies a concrete structural benchmark for a well-studied z~2 protocluster at the epoch when clusters are assembling. The homogeneous multi-band SS+BD modelling across the full JWST FoV (to ~2 R200), the explicit robustness checks (z_spec-only, stricter 1-dex passive cut, HST/WFC3 footprint restriction), and the placement against COSMOS2025, van der Wel, Ward, Martorano, Mei, Afanasiev and Delaye samples make the result useful for both observers and simulators. The ALMA-DSFG wavelength-size extension and the density–n correlation (strongest at rest-frame ~1.3 μm) are additional concrete contributions. Limitations are statistical (small passive subsample with SFRs) rather than conceptual; the paper already flags large Wilson errors in the densest bins.

major comments (2)

Sec. 2.2 and 4.2: the passive sample used for the MSR intercept and the passive–density relation is only 14 galaxies with measured SFRs (58 total with SFRs). The intermediate-intercept claim (b=0.20±0.06 vs field and cluster) and the rise to ~60% at high Σ3 are therefore carried by small-N statistics, with large Wilson errors explicitly noted in the densest bins of Fig. 6. The z_spec-only and 1-dex-below-SFMS tests (Secs. 4.2.1, 4.4, 5.2) leave slopes/intercepts and the density trend consistent, which is reassuring, but the manuscript should state more quantitatively how many objects remain in the highest-density bins under each cut and whether the intermediate-intercept offset remains significant when the passive sample is restricted to spectroscopically confirmed members only.
Secs. 2.2–2.3 and 5.2: passive galaxies are defined relative to the Speagle et al. (2014) SFMS (or log sSFR < −9.2 yr^{-1}), while the principal comparison samples (COSMOS2025/Shuntov, Martorano, Mei CARLA) use UVJ or NUV–r–J colour selection. The authors cite Nedkova et al. (2021) that MSR intercepts are largely insensitive to quiescence definition and note that both criteria isolate low-sSFR systems, but the intermediate-intercept interpretation (progenitor bias / newly quenched larger systems) is sensitive to whether the SFMS-selected sample includes the same transition objects as UVJ. A short quantitative cross-check—e.g. how many of the 14 SFMS-passive objects would be UVJ-passive if rest-frame colours were available, or an explicit statement that colours are not available for the full sample—would strengthen the claim that the offset is physical rather than selection-driven.

minor comments (6)

Table F.1 header and column labels use F444W while the text and methods consistently use F410M; this should be corrected throughout the table and any associated notes.
Fig. 2 legend and caption: the SFG intercept is quoted as b=0.63 in the text/Table 2 but appears as 0.62 in one place in Sec. 4.2.1; unify the reported values and uncertainties.
Sec. 3.1: the BD selection cut (disc size > bulge size, excluding 8 SFGs + 1 passive) is stated to span the full range of masses/sizes/n/SFR, but a one-sentence quantification (e.g. median mass or n of excluded vs retained) would make the non-bias claim easier to verify.
Appendix C / Fig. C.2: the footprint test is valuable; stating the number of passive galaxies retained in the HST/WFC3-restricted sample would help the reader judge the residual sampling uncertainty.
Fig. 5 and Sec. 4.3: the ALMA-detected subsample is small (Zhang et al. 2026); clarifying how many objects enter the median points and whether the steep wavelength gradient remains if the most extreme object is removed would be useful.
Typographical: occasional missing spaces or hyphenation (e.g. “mass–size”, “bulge–disc”) and the repeated “Article number, page N” headers are minor but should be cleaned for production.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: structural measurements and environmental trends are empirical comparisons to external benchmarks, not predictions forced by construction or self-citation.

full rationale

The paper measures single-Sérsic and bulge–disc parameters for 103 Spiderweb members with GALAPAGOS-2/GALFIT-M, fits mass–size relations of the form log(Reff) = m(log M★ − log 5e10) + b, and reports passive fractions versus Σ3. These are direct observational results compared to independent field (COSMOS2025/Shuntov, van der Wel, Ward, Martorano) and cluster (Mei, Afanasiev, Delaye) samples. Passive classification uses an SFMS cut relative to Speagle et al. (2014); the authors test a stricter 1-dex cut and a zspec-only subsample and recover consistent slopes, intercepts, and density trends. Self-citations supply membership, masses, SFRs, and ALMA context (Shimakawa, Pérez-Martínez, Zhang, Naufal) but do not define or force the structural intercepts or the passive–density rise. No equation reduces a claimed prediction to a fitted input; no uniqueness theorem or ansatz is imported to forbid alternatives. The intermediate-intercept and density-driven quenching claims are therefore empirical, not circular. Score 0 is appropriate.

Assumptions & free parameters 3 free parameters · 3 assumptions · 0 invented entities

The central claims rest on standard cosmological and stellar-population assumptions plus a small set of analysis choices (passive cut, neighbour order for density, Chebyshev polynomial orders). No new physical entities are postulated; free parameters are ordinary fit coefficients of the mass–size relations and the density estimator.

free parameters (3)

MSR slope m and intercept b (SFG and passive, each filter/component)
Linear fits log Reff = m(log M* − log 5e10) + b are obtained by bootstrap resampling of the observed sample; the intercepts are the quantities compared to field and cluster literature.
Local density estimator Σ3 (N=3 nearest neighbour)
Projected density is defined with fixed N=3; choice of N affects which local peaks are recovered and therefore the passive-fraction trend.
Passive threshold relative to SFMS
Galaxies are labelled passive if they lie ≳0.3–1 dex below the Speagle et al. main sequence (or log sSFR < −9.2); the exact threshold changes the size of the passive subsample.

assumptions (3)

domain assumption Planck 2020 cosmology (h=0.676, ΩΛ=0.685, Ωm=0.315) and Chabrier IMF
Used throughout for physical sizes, stellar masses and R200; standard but required for numerical comparison with literature.
domain assumption Single-Sérsic and two-component bulge–disc profiles adequately describe the light distribution
All structural parameters and the wavelength trends rest on the parametric models fitted by GALFIT-M.
domain assumption Narrow-band HAE/PBE selection plus spectroscopic redshifts yield a sample with only ~4% interlopers
Membership purity underpins both the mass–size and passive-density relations (Sec. 2.2).

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Cite this review

Pith. "Pith review of Mass--size evolution and the emerging passive--density relation revealed by JWST/NIRCam in the Spiderweb protocluster." pith.science (2026). https://pith.science/paper/RXFUY2JQ

@misc{pith2026260711448,
  author       = {Pith},
  title        = {Pith review of: Mass--size evolution and the emerging passive--density relation revealed by JWST/NIRCam in the Spiderweb protocluster},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/RXFUY2JQ}},
  note         = {Machine review of arXiv:2607.11448}
}

abstract

We investigate how the environment affects galaxy structure in the Spiderweb protocluster at $z=2.16$ using JWST/NIRCam F115W, F182M, and F410M imaging (rest-frame $\sim 3500${\AA} to $1.4\,\mu$m). We perform homogeneous multi-wavelength parametric modelling of the single-S\'ersic and bulge--disc decomposition for the Spiderweb member sample of 103 galaxies within the JWST field of view (up to $\sim 2\times R_{200}$). Star-forming galaxies follow a mass--size relation broadly consistent with the field, with a mildly steeper trend at the high-mass end within uncertainties. Passive galaxies exhibit a flatter mass--size relation, and their typical size (intercept at fixed stellar mass) lies between that of the coeval field and cluster passive populations, indicating an intermediate evolutionary stage. In both star-forming and passive systems, bulges are systematically more compact than discs. Galaxy sizes decrease slightly with increasing wavelength, whereas ALMA-detected dusty star-forming galaxies exhibit a much steeper wavelength dependence, consistent with centrally concentrated, obscured star formation. The passive fraction depends primarily on local density: it resembles the field at $\Sigma \lesssim 100$--$200\,{\rm gal\,Mpc^{-2}}$ and rises to $\sim60\%$ at $\Sigma \gtrsim 1000\,{\rm gal\,Mpc^{-2}}$, although with relatively large uncertainties due to the small number of galaxies in the highest-density bins, with no significant additional dependence on clustercentric distance. We also find a weak but significant correlation between local density and S\'ersic index (strongest in F410M), but no clear correlation with effective radius or the star-formation rate surface density $\Sigma_{\rm SFR}$. These results support a picture in which quenching and structural transformation are already advanced, while the size growth is still ongoing.

Figures

Figures reproduced from arXiv: 2607.11448 by the authors.

**Figure 1.** (Left) Spatial distribution of Spiderweb galaxies. Cyan squares show our parent sample, while smaller black empty squares show the rest of the galaxies in the Spiderweb protocluster, and empty small circles show member galaxies with spectroscopic confirmation. Black empty circles and squares denote SMGs from Dannerbauer et al. (2014), and passive galaxies selected using the SFMS, while the green X marker denotes X-r… view at source ↗

**Figure 2.** Mass–size relation using sizes based on a single Sérsic F182M model (rest-frame ∼ 5800 Å). Blue and red squares show SFGs and passive galaxies from the Spiderweb protocluster. Black empty circle and green X markers show SMGs and X-ray galaxies from Dannerbauer et al. (2014) and Tozzi et al. (2022). The blue dashed and red solid lines show the relation in the form log(Reff)[kpc] = m ×log(M∗)+b, using SFGs and passive… view at source ↗

**Figure 3.** Best-fit MSR intercept as a function of redshift, evaluated at M∗= 5 × 1010M⊙. Black-filled circles and squares show the intercepts of the F182M SS model (∼ 5800 Å rest-frame) for SFGs and passive galaxies from this work. Our error bars represent 68% confidence intervals based on 1 000 bootstrap resampling. Data from van der Wel et al. (2014); Mowla et al. (2019); Nedkova et al. (2021); Ward et al. (2024); Kawinwan… view at source ↗

Figures from the paper (4 more)

**Figure 4.** Figure 4: Mass–size relation for SFGs. Best fits are shown for Single Sérsic, bulge and disk components in different filters. The MSR from van der Wel et al. (2014) is shown for comparison. Bulge components are always more compact than disk components. The best-fit parameters ar…

**Figure 5.** Figure 5: Effective radius as a function of rest-frame wavelength. Black small points show the individual galaxies from our morphological sample. Large squares, circles, and triangles in black, magenta and blue show the median values for all galaxies, SFGs and passive galaxies m…

**Figure 6.** Figure 6: shows the fraction of passive (0.3 dex below the SFMS, see Sec. 2.2) galaxies as a function of increasing local density (Σ3, Sec. 3.3). We find that the passive fraction increases with density from ∼ 20% at densities of ∼ 50 [gal/Mpc2 ] (consistent with the field fra…

**Figure 7.** Figure 7: Mass–size relation. Blue and red pentagons show median values of SFGs and passive galaxies from this work. Cyan and orange diamonds show median values for field galaxies from Martorano et al. (2024) catalogue selected as described in Section 2.3. Grey shaded horizont…

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On the quenching of star formation in observed and simulated central galaxies: evidence for the role of integrated AGN feedback. , keywords =. doi:10.1093/mnras/stab3673 , archivePrefix =. 2112.07672 , primaryClass =

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Energy input from quasars regulates the growth and activity of black holes and their host galaxies. , keywords =. doi:10.1038/nature03335 , archivePrefix =. astro-ph/0502199 , primaryClass =

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Gusty, gaseous flows of FIRE: galactic winds in cosmological simulations with explicit stellar feedback. , keywords =. doi:10.1093/mnras/stv2126 , archivePrefix =. 1501.03155 , primaryClass =

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The Origin of Dwarf Galaxies, Cold Dark Matter, and Biased Galaxy Formation. , keywords =. doi:10.1086/164050 , adsurl =

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The green valley is a red herring: Galaxy Zoo reveals two evolutionary pathways towards quenching of star formation in early- and late-type galaxies. , keywords =. doi:10.1093/mnras/stu327 , archivePrefix =. 1402.4814 , primaryClass =

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Morphological Quenching of Star Formation: Making Early-Type Galaxies Red. , keywords =. doi:10.1088/0004-637X/707/1/250 , archivePrefix =. 0905.4669 , primaryClass =

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Shaping the Dust Mass-Star-formation Rate Relation. , keywords =. doi:10.1088/2041-8205/782/2/L23 , archivePrefix =. 1401.5578 , primaryClass =

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Systematics of Bulge-to-Disk Ratios. , keywords =. doi:10.1086/164015 , adsurl =

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Simulating galaxy formation with the IllustrisTNG model. , keywords =. doi:10.1093/mnras/stx2656 , archivePrefix =. 1703.02970 , primaryClass =

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The quenching and morphological evolution of central galaxies is facilitated by the feedback-driven expulsion of circumgalactic gas. , keywords =. doi:10.1093/mnras/stz3201 , archivePrefix =. 1908.11380 , primaryClass =

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Revisiting the Scaling Relations of Black Hole Masses and Host Galaxy Properties. , keywords =. doi:10.1088/0004-637X/764/2/184 , archivePrefix =. 1211.2816 , primaryClass =

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Expectations of the Size Evolution of Massive Galaxies at 3 z 6 from the TNG50 Simulation: The CEERS/JWST View. , keywords =. doi:10.3847/1538-4357/acb926 , archivePrefix =. 2208.00007 , primaryClass =

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The z 1 drop of cosmic dust abundance in a semi-analytic framework. , keywords =. doi:10.1093/mnras/stad907 , archivePrefix =. 2302.03058 , primaryClass =

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Modelling element abundances in semi-analytic models of galaxy formation. , keywords =. doi:10.1093/mnras/stt1542 , archivePrefix =. 1305.7231 , primaryClass =

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Evolution of Interstellar Medium, Star Formation, and Accretion at High Redshift. , keywords =. doi:10.3847/1538-4357/aa61a0 , archivePrefix =. 1702.04729 , primaryClass =

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Pith tools

Reviewed July 14, 2026 · model on record in the stance chip above.

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Physical conditions of the molecular gas in metal-poor galaxies

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work page Pith review arXiv doi:10.1051/0004-6361/201731000

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, keywords =

The morphologies of massive galaxies at 1 < z < 3 in the CANDELS-UDS field: compact bulges, and the rise and fall of massive discs. , keywords =. doi:10.1111/j.1365-2966.2012.22087.x , archivePrefix =. 1206.4322 , primaryClass =

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, keywords =

A large H survey at z = 2.23, 1.47, 0.84 and 0.40: the 11 Gyr evolution of star-forming galaxies from HiZELS★. , keywords =. doi:10.1093/mnras/sts096 , archivePrefix =. 1202.3436 , primaryClass =

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Dust evolution in zoom-in cosmological simulations of galaxy formation

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, keywords =

HELP: the Herschel Extragalactic Legacy Project. , keywords =. doi:10.1093/mnras/stab1526 , archivePrefix =. 2105.05659 , primaryClass =

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, keywords =

Galaxy And Mass Assembly (GAMA): Data Release 4 and the z < 0.1 total and z < 0.08 morphological galaxy stellar mass functions. , keywords =. doi:10.1093/mnras/stac472 , archivePrefix =. 2203.08539 , primaryClass =

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The Messenger , keywords =

Exploring the Universe via the Wide, Deep Near-infrared Imaging ESO Public Survey SHARKS. The Messenger , keywords =. doi:10.18727/0722-6691/5265 , archivePrefix =. 2212.09471 , primaryClass =

work page doi:10.18727/0722-6691/5265

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A dusty proto-cluster surrounding the binary galaxy HerBS-70 at $z = 2.3$

A dusty protocluster surrounding the binary galaxy HerBS-70 at z = 2.3. , keywords =. doi:10.1093/mnras/stae1155 , archivePrefix =. 2404.18991 , primaryClass =

work page Pith review arXiv doi:10.1093/mnras/stae1155