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arxiv: 2606.13781 · v2 · pith:VXAWZFRCnew · submitted 2026-06-11 · 🌌 astro-ph.GA

CANUCS/Technicolor Data Release 2: A Catalogue of Galaxy Structural Parameters in up to 29 HST+JWST bands and a Multi-Wavelength Exploration of the Galaxy Size-Mass Relation at 0.6 < z leq 4

Maya Merchant , Lamiya A. Mowla , Georgios E. Magdis , Adam Muzzin , Chris J. Willott , Roberto Abraham , Yoshihisa Asada , Maru\v{s}a Brada\v{c}
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Gabriel B. Brammer Guillaume Desprez Kartheik G. Iyer Nicholas S. Martis Ga\"el Noirot Gregor Rihtar\v{s}i\v{c} Marcin Sawicki Ghassan T. E. Sarrouh Sunna Withers Natalie Allen Jacqueline Antwi-Danso Westley Brown Jon Jude\v{z} Danilo Marchesini Rosa M. M\'erida Katherine Myers Luke Robbins Visal Sok
This is my paper

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

classification 🌌 astro-ph.GA
keywords galaxy morphologysize-mass relationJWSThigh-redshift galaxiesstructural parametersNIRCammulti-wavelength
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The pith

The slope of the galaxy size-mass relation changes with rest-frame wavelength and crosses over at a stellar mass of about 10^9.5 solar masses, proposed as the transition point between diffuse and compact morphologies.

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

The paper measures structural parameters for roughly 4100 star-forming galaxies at redshifts 0.6 to 4 using GALFIT fits across up to 29 HST and JWST bands. It introduces wavelength as a free parameter to parametrize how galaxy size depends on stellar mass and rest-frame wavelength at the same time. The central result is a reported gradient in the size-mass slope with wavelength, plus a critical crossover mass near 10^9.5 solar masses. This mass is interpreted as the scale separating galaxies that appear diffuse from those that appear compact. The work also releases the full catalog of measurements for about 41000 galaxies in the five CANUCS-Technicolor fields.

Core claim

Independent GALFIT structural fits in 19 NIRCam bands (plus HST filters) for star-forming galaxies with 8.5 < log(M*/M⊙) ≤ 11.5 show a gradient in the slope of the size-mass relation as a function of rest-frame wavelength, with a critical crossover mass at ∼10^9.5 M⊙ that is proposed as the stellar mass separating diffuse from compact galaxy morphologies.

What carries the argument

Multi-band size-mass relation with wavelength treated as a free parameter, derived from independent GALFIT measurements in each of up to 29 filters.

If this is right

  • Below the crossover mass, galaxy sizes appear more extended at shorter wavelengths; above it, sizes appear more compact across wavelengths.
  • The size-mass relation can be written as a single function of both mass and wavelength rather than separate relations at fixed wavelength.
  • The characteristic mass may mark a shift in the dominant structural component or assembly process.
  • The public catalog allows the same wavelength-dependent analysis to be repeated in other fields or with additional filters.

Where Pith is reading between the lines

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

  • This mass scale might align with other known transitions in galaxy properties, such as changes in star-formation efficiency or bulge-to-disk ratio.
  • Extending the analysis to rest-frame UV or mid-infrared bands could test whether the slope gradient continues or saturates.
  • If the crossover is physical, targeted observations of galaxies near 10^9.5 solar masses could reveal whether morphological change coincides with changes in kinematics or gas content.

Load-bearing premise

GALFIT sizes measured separately in each band accurately reflect intrinsic galaxy sizes without major systematic errors from wavelength-dependent effects such as dust attenuation or stellar population gradients.

What would settle it

Re-measuring the same galaxies with a size estimator that explicitly corrects for dust and stellar-population gradients across wavelengths and finding no remaining slope gradient with wavelength.

Figures

Figures reproduced from arXiv: 2606.13781 by Adam Muzzin, Chris J. Willott, Danilo Marchesini, Gabriel B. Brammer, Ga\"el Noirot, Georgios E. Magdis, Ghassan T. E. Sarrouh, Gregor Rihtar\v{s}i\v{c}, Guillaume Desprez, Jacqueline Antwi-Danso, Jon Jude\v{z}, Kartheik G. Iyer, Katherine Myers, Lamiya A. Mowla, Luke Robbins, Marcin Sawicki, Maru\v{s}a Brada\v{c}, Maya Merchant, Natalie Allen, Nicholas S. Martis, Roberto Abraham, Rosa M. M\'erida, Sunna Withers, Visal Sok, Westley Brown, Yoshihisa Asada.

Figure 1
Figure 1. Figure 1: RGB mosaics of the five CANUCS NIRCam Flanking Fields (NCF): MACS J1423, MACS J0417, Abell 370, MACS J0416, and MACS J1149. The RGB images are created from the combination of F090W + F115W + F150W (blue), F182M + F210M + F277W (green), and F335M + F360M + F444W (red) filters. Each pair of squares represents the two NIRCam modules, each covering approximately 2.2 ′ × 2.2 ′ on the sky. The CANUCS survey prov… view at source ↗
Figure 2
Figure 2. Figure 2: Left: Images of a single galaxy (CANUCS-A370-2200379; log(M∗/M⊙) = 10.46 ± 0.001, z = 1.66 ± 0.048) across 19 NIRCam filters shown by their waverange. Right: Associated parameters of effective radius, S´ersic index, and magnitude as a function of observed wavelength for this galaxy. The mean (µ; dashed horizontal line) and standard error (σ) is included for each variable. While all available imaging is use… view at source ↗
Figure 3
Figure 3. Figure 3: shows the resulting UVJ distribution of the sample, with quiescent and star-forming galaxies indi￾cated. This selection yields 563 quiescent and 6,138 star￾forming galaxies with a quiescent fraction of ∼ 8.5%, slightly lower than predicted compared to expectations of ∼ 10−20% quenched up to Cosmic Noon, z = 3.5 (A. Muzzin et al. 2013). The distributions of photometric redshift, stellar mass, and specific s… view at source ↗
Figure 4
Figure 4. Figure 4: The size–mass relation of star-forming galaxies at the rest-frame 0.5µm (top) and 1.5 µm (bottom) between 0.6 < z ≤ 4 and 8.5 < log(M∗/M⊙) ≤ 11.5. Data points are shown in grey with best-fits lines overplotted (with the dashed portion representing extrapolation below the mass completeness limit) and the 1σ intrinsic scatter is shaded. The black dashed line shows the slope of the lowest redshift bin, 0.6 < … view at source ↗
Figure 6
Figure 6. Figure 6: Best-fit size–mass relations for star-forming galaxies in each redshift bin at rest-frame 0.5 µm (top) com￾pared to K. V. Nedkova et al. 2021 (N+21) and N. Allen et al. 2024 (A+24), and at the rest-frame 1.5 µm (bottom) compared to M. Martorano et al. 2024 (M+24). Dashed lines represent extrapolations and shaded regions indicate the 1σ intrinsic scatter. 4.2. Size–Wavelength Relation by Redshift and Mass W… view at source ↗
Figure 7
Figure 7. Figure 7: Top (a): the size–wavelength relation as a function of stellar mass at fixed redshift (2 < z ≤ 4), colour-coded by mass bin. Bottom (b): the size–wavelength relation as a function of redshift at fixed stellar mass (8.5 ≤ log(M∗/M⊙) < 9.5), colour-coded by redshift bin and compared to N. Allen et al. (2024) at z ≥ 3. Panel (c): weighted average size–wavelength relations for star-forming galaxies at 0.6 < z … view at source ↗
Figure 8
Figure 8. Figure 8: Best-fit coefficients of the weighted least-squares regression as a function of rest-frame wavelength bin median: the mass coefficient m(λ) (left), the redshift coefficient z(λ) (center), and the constant term K(λ) (right), with 1σ uncer￾tainties. Purple lines show the best-fit power-law (mass and constant terms) and linear (redshift term) functional forms over 0.25µm < λRF < 2.0µm with a 1σ confidence int… view at source ↗
Figure 9
Figure 9. Figure 9: The multi-wavelength size–mass relation for star-forming galaxies at 0.6 < z ≤ 4, shown in each of the 11 selected JWST/NIRCam filters colour-coded by wavelength. Upper panels show the density contours of individual best-fit size–mass measurements; lower panels show the LinMix linear best-fits in each redshift bin. The dashed vertical line indicates the characteristic mass per redshift bin at which the siz… view at source ↗
Figure 10
Figure 10. Figure 10: Ratio of the rest-frame 1 µm to rest-frame 0.5 µm effective radius as a function of stellar mass, mea￾sured using F360M and F182M respectively. A ratio below unity indicates that galaxies are more extended at shorter wavelengths. underlying stellar mass distribution (E. F. Bell et al. 2003; A. van der Wel et al. 2014). Radial colour gradients in star-forming galaxies are well established observationally, … view at source ↗
Figure 11
Figure 11. Figure 11: shows the distributions of photometric redshift, stellar mass, and specific star formation rate (sSFR) for the star-forming and quiescent subsamples identified via UVJ selection (Section 3.3). The star-forming sample spans 0.6 < z ≤ 4 and 8.5 < log(M∗/M⊙) ≤ 11.5, with the bulk of the population at log(M∗/M⊙) ∼ 9–10. The quiescent sample is distributed to higher stellar masses and lower sSFR values, as exp… view at source ↗
Figure 12
Figure 12. Figure 12: shows an example of the single-component GALFIT fitting output for a representative galaxy (CANUCS￾A370-2200497; log(M∗/M⊙) = 9.02 ± 0.121, z = 1.99 ± 0.101) across available JWST/NIRCam filters across the full wavelength range used in this analysis. For each filter, three panels are shown from top to bottom: the background￾subtracted science image with neighbouring sources masked (in white), the best-fit… view at source ↗
Figure 13
Figure 13. Figure 13: Stellar mass as a function of photometric redshift for star-forming galaxies in the five CANUCS NIRCam flanking fields between 0.6 < z ≤ 4. The median (solid), 16th, and 84th percentile (dashed) stellar mass completeness limits estimated following R. M. M´erida et al. (2026) are shown in purple, and completeness limits outlined in Equation 2 are adopted. Wavelength Bin (µm) Number of Measurements Waveleng… view at source ↗
Figure 14
Figure 14. Figure 14: Residuals ∆ log Reff = log Reff, obs − log Reff, pred between observed and predicted effective radii from Equation 9 as a function of rest-frame wavelength. Points show the weighted mean residual in each wavelength bin and error bars indicate the weighted standard deviation. The dashed line at ∆ log Reff = 0 indicates perfect agreement. The intrinsic scatter of ±0.05 dex and mean offset of µ∆ = 0.01 dex c… view at source ↗
Figure 15
Figure 15. Figure 15: shows the S´ersic index n as a function of stellar mass measured in F277W for star-forming galaxies per redshift bin; we utilize F277W as it is the deepest filter available in the CANUCS-Technicolor dataset and provides the highest S/N morphological measurements, minimizing the contribution of fitting noise to the observed trends. The crossover mass identified in Section 4.4 is overplotted in each panel a… view at source ↗
Figure 16
Figure 16. Figure 16: V -band dust attenuation AV as a function of stellar mass for star-forming galaxies in the four redshift bins (0.6 < z ≤ 1.0, 1.0 < z ≤ 1.5, 1.5 < z ≤ 2.0, and 2.0 < z ≤ 4.0), shown in increasingly lighter shades of grey. AV values are derived from Dense Basis SED fitting. The dashed vertical lines at log(M∗/M⊙) = 9 and 10 bracket the mass range over which AV increases sharply, coinciding with the crossov… view at source ↗
read the original abstract

We present James Webb Space Telescope (JWST) results of a morphological study of galaxies in the CAnadian NIRISS Unbiased Cluster (CANUCS) and Technicolor surveys, observed in 19 medium- and broadband NIRCam filters in five CANUCS NIRCam Flanking Fields with rest-frame wavelength coverage between $\sim 0.2 - 3.2\mu m$. Using GALFIT, we measure the morphological parameters of $\sim$ 4,100 star-forming galaxies at $0.6 < z \leq 4$ with stellar masses of $8.5 < \text{log}(M_*/M_\odot) \leq 11.5$. This enables us to concurrently examine how galaxy size varies as a function of stellar mass, redshift, and rest-frame wavelength to provide a novel parametrization of the galaxy size-wavelength relation. Additionally, we analyze the evolution of the galaxy size-mass relation in the rest-frame optical and NIR with the introduction of wavelength as a free parameter. We report a gradient in the slope of the size-mass relation with respect to rest-frame wavelength with a critical crossover mass at $\sim 10^{9.5} M_\odot$. We propose this characteristic mass as the stellar mass at which galaxies transition between diffuse and compact morphologies. We concurrently present the data release of morphological measurements of the five CANUCS-Technicolor NIRCam Flanking Fields in which we provide structural parameters for $\sim$ 41,000 galaxies in up to 29 JWST+HST filters.

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 releases a catalog of galaxy structural parameters measured with GALFIT for ~41,000 galaxies across up to 29 HST+JWST bands in the CANUCS/Technicolor NIRCam Flanking Fields. For a subsample of ~4,100 star-forming galaxies at 0.6 < z ≤ 4 (8.5 < log(M*/M⊙) ≤ 11.5), it parametrizes the size-mass relation as a function of stellar mass, redshift, and rest-frame wavelength (0.2–3.2 μm), reporting a gradient in the size-mass slope with wavelength and a crossover mass of ~10^9.5 M⊙ interpreted as the transition between diffuse and compact morphologies.

Significance. If the wavelength-dependent size measurements are shown to be free of major systematic biases, the work supplies a new empirical parametrization of the size-wavelength relation and identifies a characteristic mass scale potentially linked to morphological transitions. The public release of multi-band structural parameters for a large sample is a concrete contribution to the community.

major comments (2)
  1. [GALFIT structural-parameter measurements (methods section describing per-band fits)] The central result (wavelength gradient in size-mass slope and crossover mass at ~10^9.5 M⊙) rests on the assumption that independent single-component GALFIT fits performed separately in each of the 19 NIRCam bands return effective radii that faithfully trace intrinsic galaxy size at that rest-frame wavelength. No joint multi-band fitting, explicit color-gradient modeling, or quantitative tests for dust attenuation or stellar-population effects are described; such biases are expected to be stronger below the reported crossover mass and could artificially steepen the reported slope gradient.
  2. [Results on size-mass relation and wavelength dependence] The manuscript provides no quantitative assessment of sample completeness as a function of mass and wavelength, GALFIT convergence criteria, or robustness checks (e.g., comparison of r_e across adjacent bands or against mock galaxies with known gradients). These omissions make it impossible to evaluate whether the reported slope gradient and crossover mass are robust or driven by selection or fitting artifacts.
minor comments (2)
  1. [Abstract] The abstract states the main result but omits any mention of uncertainties on the crossover mass, sample size per redshift bin, or fitting-quality metrics.
  2. [Data Release] Clarify in the data-release section how many of the ~41,000 galaxies have converged fits in all 29 bands versus subsets, and provide a table summarizing the wavelength coverage per object.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed comments. We address each major comment below, agreeing that additional validation is needed, and will incorporate the suggested improvements in the revised manuscript.

read point-by-point responses

  1. Referee: [GALFIT structural-parameter measurements (methods section describing per-band fits)] The central result (wavelength gradient in size-mass slope and crossover mass at ~10^9.5 M⊙) rests on the assumption that independent single-component GALFIT fits performed separately in each of the 19 NIRCam bands return effective radii that faithfully trace intrinsic galaxy size at that rest-frame wavelength. No joint multi-band fitting, explicit color-gradient modeling, or quantitative tests for dust attenuation or stellar-population effects are described; such biases are expected to be stronger below the reported crossover mass and could artificially steepen the reported slope gradient.

    Authors: We agree that the manuscript relies on independent per-band GALFIT fits without joint multi-band modeling or explicit tests for dust/stellar-population biases, which is a limitation. While such fits follow standard practice for wavelength-dependent studies, we will add a new methods subsection discussing these potential systematics and include quantitative tests (adjacent-band r_e comparisons and mock galaxies with known gradients) to assess their impact, particularly below the crossover mass. This will better support the interpretation of the slope gradient. revision: yes

  2. Referee: [Results on size-mass relation and wavelength dependence] The manuscript provides no quantitative assessment of sample completeness as a function of mass and wavelength, GALFIT convergence criteria, or robustness checks (e.g., comparison of r_e across adjacent bands or against mock galaxies with known gradients). These omissions make it impossible to evaluate whether the reported slope gradient and crossover mass are robust or driven by selection or fitting artifacts.

    Authors: We acknowledge that the current manuscript omits explicit quantitative assessments of completeness (vs. mass/wavelength), GALFIT convergence statistics, and robustness checks. In revision we will expand the results and methods sections to include these: completeness simulations, convergence criteria, band-to-band r_e comparisons, and mock-galaxy tests. These additions will enable readers to evaluate the robustness of the size-mass parametrization and crossover mass. revision: yes

Circularity Check

0 steps flagged

No circularity: empirical catalog trends from independent multi-band fits

full rationale

The paper extracts structural parameters via independent GALFIT fits per band on observed imaging, then reports measured trends in the size-mass slope versus rest-frame wavelength and a crossover mass scale. No equations, fitted parameters, or self-citations are shown that reduce the reported gradient or 10^9.5 M_⊙ crossover back to the input data by construction. The derivation chain consists of direct observational measurements and statistical trends on the catalog; it remains self-contained against external benchmarks with no load-bearing self-definition or renaming of known results.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 1 invented entities

The paper is observational and relies on standard fitting software plus an interpretive mass scale derived from data trends.

free parameters (1)
  • crossover mass = ~10^{9.5} M_⊙
    The ~10^9.5 M_⊙ value is identified from the change in slope of the fitted size-mass relation across wavelengths.
axioms (1)
  • domain assumption GALFIT provides reliable structural parameters across a wide rest-frame wavelength range
    All size measurements and the subsequent size-mass analysis depend on the outputs of this fitting tool being unbiased in each band.
invented entities (1)
  • characteristic mass as morphological transition point no independent evidence
    purpose: To interpret the observed crossover in the size-mass slope as the stellar mass separating diffuse from compact galaxy morphologies
    This is a proposed physical meaning assigned to the fitted crossover mass without additional independent evidence cited in the abstract.

pith-pipeline@v0.9.1-grok · 5988 in / 1385 out tokens · 30222 ms · 2026-06-27T06:06:11.454340+00:00 · methodology

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