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In the Spiderweb protocluster at z=2.16, quenching and structural change are already advanced while size growth is still ongoing.

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2026-07-14 05:31 UTC pith:RXFUY2JQ

load-bearing objection Solid JWST structural census of Spiderweb: intermediate passive MSR intercept and local-density-driven passive fraction, limited mainly by small passive N. the 2 major comments →

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

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

J. Nadolny , J. M. P\'erez-Mart\'inez , H. Dannerbauer , B. Haussler , M. Huertas-Company , K. Daikuhara , T. Kodama , Y. Koyama
show 3 more authors
A. Naufal P. G. P\'erez-Gonz\'alez Y. H. Zhang
This is my paper
classification astro-ph.GA
keywords protoclustermass-size relationpassive-density relationJWST/NIRCamgalaxy structureenvironmental quenchingbulge-disc decompositionSpiderweb
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

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.

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.

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.

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.

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.

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

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

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)
  1. 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.
  2. 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)
  1. 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.
  2. 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.
  3. 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.
  4. 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.
  5. 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.
  6. 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

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.

Axiom & Free-Parameter Ledger

3 free parameters · 3 axioms · 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.
axioms (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).

pith-pipeline@v1.1.0-grok45 · 38222 in / 2748 out tokens · 27788 ms · 2026-07-14T05:31:24.427362+00:00 · methodology

0 comments
read the original 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 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, Y. Koyama.

Figure 1
Figure 1. 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 d… view at source ↗
Figure 2
Figure 2. 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 a… view at source ↗
Figure 3
Figure 3. 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 inter￾vals 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)… view at source ↗
Figure 4
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 are given in [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
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 measured for a single Sérsic model, bulge and disk components. Cyan left-triangles show ALMA-detected subsample from Zhang et al. (2026). cle… view at source ↗
Figure 6
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 lo￾cal density (Σ3, Sec. 3.3). We find that the passive frac￾tion increases with density from ∼ 20% at densities of ∼ 50 [gal/Mpc2 ] (consistent with the field fraction) to about 60% at ∼ 1100 [gal/Mpc2 ]. This is consistent with results from the CLARA survey (Wylezalek et al. 2013) at z between 1.9 an… view at source ↗
Figure 7
Figure 7. Figure 7: Mass–size relation. Blue and red pentagons show median val￾ues 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 hor￾izontally and vertically hatched regions show LTGs and ETGs MSR from van der Wel et al. (2014). Dotted black line is the MSR for SFG from cluster… view at source ↗

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