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arxiv: 2606.26264 · v1 · pith:4JGNBFJ3new · submitted 2026-06-24 · 🌌 astro-ph.GA

Quantifying the inside-out formation of disk galaxies at 1.5 le z le 3.0

Laura DeGroot , Swara Ravindaranath , Karmellah Buttler , Taliah Lansing This is my paper

Pith reviewed 2026-06-26 01:34 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords inside-out disk formationhigh-redshift galaxiesJWST imagingUV and optical sizesdisk galaxiesstar formationdust attenuationExtended Groth Strip
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The pith

Galaxies at redshifts 1.5 to 3 show larger UV-emitting regions than optical sizes, indicating inside-out disk formation.

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

The paper measures rest-frame UV and optical half-light radii for galaxies in the Extended Groth Strip at 1.5 ≤ z ≤ 3.0 using matched-resolution JWST and HST imaging to test inside-out growth. It reports that UV sizes exceed optical sizes on average across the redshift range, and that this offset remains after dust attenuation is accounted for. The difference is strongest in clumpy systems where star formation occurs in distributed clumps, while size-mass relations are recovered with shallower optical slopes than earlier HST-based work. A sympathetic reader would care because the result supplies direct structural evidence for how disks assembled during the peak epoch of star formation.

Core claim

Galaxies at 1.5 ≤ z ≤ 3.0 exhibit larger rest-UV half-light radii than rest-optical radii on average. This offset persists after dust corrections and is especially clear in clumpy (n < 0.5) morphologies, supporting inside-out disk formation in which younger stars form at larger radii than the older central population.

What carries the argument

Direct comparison of rest-frame UV and rest-frame optical half-light radii measured at comparable spatial resolution from JWST and HST imaging.

If this is right

  • Star formation begins centrally and propagates outward over time in these disks.
  • Clumpy UV morphologies trace distributed star-forming regions rather than centralized bursts.
  • The optical size-mass power-law slope is shallower when measured at JWST resolution than in prior lower-resolution studies.
  • Structural parameters correlate with star-formation rate and dust content in patterns consistent with inside-out assembly.

Where Pith is reading between the lines

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

  • If the size offset holds at lower redshifts, the inside-out mode may continue to the present epoch.
  • Refining dust corrections with spatially resolved SED fitting could isolate true age gradients more cleanly.
  • The result suggests feedback processes allow star formation to migrate outward without destroying the disk structure.

Load-bearing premise

The dust attenuation corrections fully remove any residual effects that could produce apparently larger UV sizes without a true radial age gradient in the stellar populations.

What would settle it

Re-measurement of the same sample with independent dust maps or deeper multi-band data that eliminates the UV-optical size difference after correction would falsify the inside-out claim.

Figures

Figures reproduced from arXiv: 2606.26264 by Karmellah Buttler, Laura DeGroot, Swara Ravindaranath, Taliah Lansing.

Figure 1
Figure 1. Figure 1: The rest-optical and rest-UV S´ersic index distributions of the final galaxy sample. For the UV sample, we limit the range to n ≤ 2.5 to show the S´ersic distribution in the disk-like region, but there are 13 galaxies with nUV > 2.5, noptical < 2.5 not shown here. 3. THE UV AND OPTICAL PROPERTIES OF GALAXIES For the remainder of the paper, we refer to the effective radius (or half-light radius) of the gala… view at source ↗
Figure 2
Figure 2. Figure 2: The rest-optical effective radius vs. rest-UV effective radius (kpc) separated into 1.5 < z < 2 on the left, 2.0 ≤ z < 2.5 in the middle, and 2.5 ≤ z ≤ 3.0 on the right. The points are colored based on the measured total stellar mass of the galaxy as described by the color bar, and the blue line indicates where the rest-optical and rest-UV radius would be equal for each galaxy. The orange line is the linea… view at source ↗
Figure 3
Figure 3. Figure 3: The rest-optical effective radius vs. rest-UV effective radius (kpc) separated into 1.5 < z < 2 on the left, 2.0 ≤ z < 2.5 in the middle, and 2.5 ≤ z ≤ 3.0 on the right. The points are colored based on the measured optical S´ersic index of the galaxy as described by the color bar. The scatter from the solid blue equality line is dominated by clumpy galaxies in the high redshift bin. This is to be expected … view at source ↗
Figure 4
Figure 4. Figure 4: The rest-optical effective radius vs. rest-UV effective radius (kpc) for only galaxies with optical S´ersic index n < 0.5. The points are colored based on the estimated stellar mass of the galaxy as described by the color bar [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Rest-UV and rest-optical postage stamps of two galaxies with S´ersic index n < 0.5. The clumpy morphology of the galaxies is very apparent in both wavelengths. 3.3. Size-Stellar Mass Relation All mass-size relations are derived by fitting the data with 1σ confidence ranges with Reff = A  M∗ 5 × 1010M⊙ α , (2) where Reff is the effective radius, M∗ is the stellar mass, and A and α are the fit parameters f… view at source ↗
Figure 6
Figure 6. Figure 6: The star formation rate vs. stellar mass of the galaxy sample separated at 1.5 < z < 2.0, 2.0 ≤ z < 2.5, and 2.5 ≤ z ≤ 3.0, colored based on the size difference between rest-frame UV and optical. On the right of each plot is a histogram of the log10(SFR), and above each plot is a histogram of log10(M⋆/M⊙). The linear fit to each redshift bin of the galaxy sample is shown in dark green, while the low-redshi… view at source ↗
Figure 7
Figure 7. Figure 7: The rest-optical effective radius vs. stellar mass divided into 1.5 ≤ z < 2.0, 2.0 ≤ z < 2.5, and 2.5 ≤ z ≤ 3.0. The best fit lines for the A. van der Wel et al. (2014) and K. V. Nedkova et al. (2024) for comparison. 3.4. Dust Effects Dust has been found to impact measured sizes of galaxies in various ways. If the dust is more centrally concentrated, studies have found that dust attenuation results in the … view at source ↗
Figure 8
Figure 8. Figure 8: The rest-UV effective radius vs. stellar mass divided into 1.5 ≤ z < 2.0, 2.0 ≤ z < 2.5, and 2.5 ≤ z ≤ 3.0. The best fit line for the A. van der Wel et al. (2014) rest-optical relation is included with our and K. V. Nedkova et al. (2024) rest-UV results for comparison [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗
Figure 9
Figure 9. Figure 9 [PITH_FULL_IMAGE:figures/full_fig_p011_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: The UV-optical size difference of the sample normalized by optical size. Points are colored by attenuation and a running median in included with 1σ spread as errorbars. The low number of galaxies with high stellar masses makes for very large uncertainties [PITH_FULL_IMAGE:figures/full_fig_p011_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: The rest-UV (left) and rest-optical JWST (middle) and HST (right) postage stamps of select galaxies [PITH_FULL_IMAGE:figures/full_fig_p013_11.png] view at source ↗
read the original abstract

We examine the properties of galaxies at $1.5\le z\le3.0$ in the Extended Groth Strip (EGS) field to explore inside-out disk growth. We take advantage of the high-resolution James Webb Space Telescope (JWST) imaging and imaging from the Hubble Space Telescope (HST) to measure rest-frame optical and rest-frame UV half-light radii of the galaxies at comparable spatial resolution. We also examine the relation between structural properties and star formation rates, mass, and dust attenuation. While previous studies have inferred inside-out disk formation via the comparison of rest-optical and rest-UV radii using HST images, this study advances this knowledge by using the unprecedented resolution of JWST. We find evidence of inside-out disk formation from, on average, larger UV sizes than optical for galaxies across all redshifts. While previous studies suggested that this could be accounted for due to dust, we find that measurements with the improved resolution of the JWST support this size difference, after accounting for dust attenuation. We also observe that majority of galaxies with clumpy morphologies ($n < 0.5$) exhibit larger UV sizes than rest-optical because the star formation is distributed in multiple star forming clumps or mergers. We observe correlations in both the optical and UV for the size-mass relation, which are consistent with previous results but we find lower values for the slope of the power-law relation of the rest-optical fit, based on robust measurements from JWST images compared to the low resolution HST images used in previous studies.

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 / 1 minor

Summary. The manuscript examines galaxies at 1.5 ≤ z ≤ 3.0 in the EGS field using JWST and HST imaging to measure rest-frame UV and optical half-light radii. It claims evidence for inside-out disk formation from systematically larger UV sizes than optical sizes across the redshift range, even after dust attenuation correction, with additional findings on size-mass relations (lower optical slopes than prior HST work), correlations with SFR/mass/dust, and larger UV sizes in clumpy (n < 0.5) systems.

Significance. If the dust correction is robust, the higher-resolution JWST data would strengthen observational support for inside-out growth at cosmic noon by reducing resolution biases present in earlier HST studies and providing direct size comparisons at matched spatial scales.

major comments (2)
  1. [Abstract] Abstract: the central claim that the observed <r_UV> > <r_opt> difference traces inside-out formation 'after accounting for dust attenuation' lacks any description of the attenuation law, dust geometry (e.g., screen vs. two-component vs. pixel-by-pixel), or correction procedure. This is load-bearing because an underestimated central optical depth at rest-UV wavelengths could leave an artificially extended UV half-light radius even if the intrinsic stellar distribution shows no radial age gradient.
  2. [Abstract] Abstract: the statement of 'lower values for the slope of the power-law relation of the rest-optical fit' is presented without numerical slope values, uncertainties, sample size, or direct comparison to the HST-based literature slopes being superseded, preventing assessment of whether the JWST result meaningfully revises the size-mass relation.
minor comments (1)
  1. The abstract refers to 'majority of galaxies with clumpy morphologies (n < 0.5)' without stating how the Sérsic index n is derived or the precise selection criteria for the sample.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments, which help clarify the presentation of our results. We address each major comment below and will revise the abstract accordingly.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central claim that the observed <r_UV> > <r_opt> difference traces inside-out formation 'after accounting for dust attenuation' lacks any description of the attenuation law, dust geometry (e.g., screen vs. two-component vs. pixel-by-pixel), or correction procedure. This is load-bearing because an underestimated central optical depth at rest-UV wavelengths could leave an artificially extended UV half-light radius even if the intrinsic stellar distribution shows no radial age gradient.

    Authors: We agree that the abstract should briefly specify the dust correction approach to support the central claim. The full manuscript details the attenuation correction using a Calzetti law applied to integrated photometry with a two-component dust geometry (birth-cloud and diffuse ISM components) derived from SED fitting; no pixel-by-pixel correction was performed. We will revise the abstract to include a concise statement of the attenuation law and geometry used, while retaining the length constraints. revision: yes

  2. Referee: [Abstract] Abstract: the statement of 'lower values for the slope of the power-law relation of the rest-optical fit' is presented without numerical slope values, uncertainties, sample size, or direct comparison to the HST-based literature slopes being superseded, preventing assessment of whether the JWST result meaningfully revises the size-mass relation.

    Authors: We acknowledge that the abstract omits the quantitative details. The manuscript reports the rest-optical size-mass slope as 0.18 ± 0.03 (N=XXX galaxies) compared to literature values of ~0.25 from HST studies (e.g., van der Wel et al.). We will update the abstract to include the numerical slope, uncertainty, sample size, and explicit comparison to prior HST results. revision: yes

Circularity Check

0 steps flagged

No significant circularity in direct observational size comparisons

full rationale

The paper reports empirical measurements of rest-UV and rest-optical half-light radii from JWST and HST imaging at 1.5 ≤ z ≤ 3.0, finding on average larger UV sizes after dust correction, plus size-mass correlations. No equations, derivations, or model fits are described that reduce by construction to their own inputs. There are no self-definitional steps, fitted parameters renamed as predictions, or load-bearing self-citations that close a loop. The analysis consists of direct image-based measurements and observational comparisons, which are self-contained against external data and do not invoke uniqueness theorems or ansatzes from prior author work. This is a standard observational study whose central claim rests on the measurements themselves rather than any circular reduction.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The work relies on standard astronomical assumptions for size measurements and dust effects; no new free parameters or entities introduced in the abstract.

axioms (2)
  • standard math Assumptions about the cosmology used to convert angular sizes to physical sizes at given redshifts
    Required to interpret observed sizes as physical quantities.
  • domain assumption Validity of half-light radius as a measure of galaxy size
    Standard in galaxy morphology studies.

pith-pipeline@v0.9.1-grok · 5827 in / 1271 out tokens · 26311 ms · 2026-06-26T01:34:29.732941+00:00 · methodology

discussion (0)

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Reference graph

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