Pith. sign in

REVIEW 2 major objections 1 minor 106 references

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

T0 review · 2 major / 1 minor · reviewed 2026-06-26 · grok-4.3

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read Galaxies at redshifts 1.5 to 3 show larger UV-emitting regions than optical sizes, indicating inside-out disk formation.

desk verdict This mostly reconfirms the HST-era inside-out growth signal with JWST resolution in one field, but the dust correction step is underspecified. read the letter →

arxiv 2606.26264 v1 pith:4JGNBFJ3 submitted 2026-06-24 astro-ph.GA

Laura DeGroot , Swara Ravindaranath , Karmellah Buttler , Taliah Lansing This is my paper · ORCID
classification astro-ph.GA
keywords inside-outdiskformationhigh-redshiftgalaxiesJWSTimagingUVandopticalsizesstardustattenuationExtendedGrothStrip
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

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.

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.

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.

Watch

Extended reading notes

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.

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.

Editorial extensions

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.

Reading between the lines

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.
Share X Bluesky LinkedIn Reddit HN

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 / 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 · score 0.0 of 10

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.

Assumptions & free parameters 0 free parameters · 2 assumptions · 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.

assumptions (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.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Quantifying the inside-out formation of disk galaxies at $1.5 \le z \le 3.0$." pith.science (2026). https://pith.science/paper/4JGNBFJ3

@misc{pith2026260626264,
  author       = {Pith},
  title        = {Pith review of: Quantifying the inside-out formation of disk galaxies at $1.5 \le z \le 3.0$},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/4JGNBFJ3}},
  note         = {Machine review of arXiv:2606.26264}
}
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.

Figures

Figures reproduced from arXiv: 2606.26264 by the authors.

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 galaxy as the … view at source ↗
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 linear-best fit… view at source ↗
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 if the vio… view at source ↗
Figures from the paper (8 more)
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]
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 ra…
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 eac…
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 meas…
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 …
Figure 9
Figure 9. Figure 9 [PITH_FULL_IMAGE:figures/full_fig_p011_9.png]
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_…
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]

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

106 extracted references · 103 canonical work pages

  1. [1]

    , archivePrefix = "arXiv", eprint =

    Common-. Publications of the Astronomical Society of the Pacific , author =. 2011 , note =. doi:10.1086/662219 , abstract =

    work page doi:10.1086/662219 2011

  2. [2]

    The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package

    The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package. , keywords =. doi:10.3847/1538-3881/aabc4f , archivePrefix =. 1801.02634 , primaryClass =

    work page Pith review arXiv doi:10.3847/1538-3881/aabc4f

  3. [3]

    Astropy: A Community Python Package for Astronomy

    Astropy: A community Python package for astronomy. , keywords =. 2013. doi:10.1051/0004-6361/201322068 , archivePrefix =. 1307.6212 , primaryClass =

    work page Pith review arXiv doi:10.1051/0004-6361/201322068 2013

  4. [4]

    B., Finkelstein, S

    CEERS Epoch 1 NIRCam Imaging: Reduction Methods and Simulations Enabling Early JWST Science Results. , keywords =. doi:10.3847/2041-8213/acbb08 , archivePrefix =. 2211.02495 , primaryClass =

    work page doi:10.3847/2041-8213/acbb08

  5. [5]

    MNRAS , author =

    GALAPAGOS: from pixels to parameters. , keywords =. doi:10.1111/j.1365-2966.2012.20619.x , archivePrefix =. 1203.1831 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.20619.x 2012

  6. [6]

    G., Cava, A., et al

    The CANDELS/SHARDS Multiwavelength Catalog in GOODS-N: Photometry, Photometric Redshifts, Stellar Masses, Emission-line Fluxes, and Star Formation Rates. , keywords =. doi:10.3847/1538-4365/ab23f2 , archivePrefix =. 1908.00569 , primaryClass =

    work page doi:10.3847/1538-4365/ab23f2 1908

  7. [7]

    DYNAMO II: Coupled Stellar and Ionized Gas Kinematics in Two Low Redshift Clumpy Disks

    DYNAMO - II. Coupled stellar and ionized-gas kinematics in two low-redshift clumpy discs. , keywords =. doi:10.1093/mnras/stu1029 , archivePrefix =. 1405.6753 , primaryClass =

    work page Pith review arXiv doi:10.1093/mnras/stu1029

  8. [8]

    What turns galaxies off? The different morphologies of star-forming and quiescent galaxies since z~2 from CANDELS

    What Turns Galaxies Off? The Different Morphologies of Star-forming and Quiescent Galaxies since z -0.5ex 2 from CANDELS. , keywords =. doi:10.1088/0004-637X/753/2/167 , archivePrefix =. 1110.3786 , primaryClass =

    work page Pith review arXiv doi:10.1088/0004-637x/753/2/167

Show all 106 references
  1. [9]

    , keywords =

    JWST Reveals Bulge-dominated Star-forming Galaxies at Cosmic Noon. , keywords =. doi:10.3847/2041-8213/ad7e27 , archivePrefix =. 2409.08328 , primaryClass =

    doi

  2. [10]

    , keywords =

    SExtractor: Software for source extraction. , keywords =. doi:10.1051/aas:1996164 , adsurl =

    doi

  3. [11]

    , keywords =

    Rapid Formation of Exponential Disks and Bulges at High Redshift from the Dynamical Evolution of Clump-Cluster and Chain Galaxies. , keywords =. doi:10.1086/522077 , archivePrefix =. 0708.0306 , primaryClass =

    doi arXiv

  4. [12]

    , keywords =

    The Thick Disks of Spiral Galaxies as Relics from Gas-rich, Turbulent, Clumpy Disks at High Redshift. , keywords =. doi:10.1088/0004-637X/707/1/L1 , archivePrefix =. 0910.3677 , primaryClass =

    doi arXiv

  5. [13]

    and Robitaille, T

    Bradley, Larry and Sipőcz, Brigitta M. and Robitaille, T. P. and Tollerud, E. J. and Vinícius, Zé and Deil, Christoph and Barbary, Kyle and Wilson, Tom J. and Busko, Ivo and Donath, Axel and Günther, Hans Moritz and Cara, Mihai and Lim, P. L. and Meßlinger, Sebastian and Conse...

    doi

  6. [14]

    Astronomy & Astrophysics , author =

    Convolution kernels for multi-wavelength imaging , volume =. Astronomy & Astrophysics , author =. 2016 , note =. doi:10.1051/0004-6361/201629080 , abstract =

    2016 doi

  7. [15]

    Spectroscopic clues to the origin and evolution of chain galaxies

    Observations and modeling of a clumpy galaxy at z = 1.6. Spectroscopic clues to the origin and evolution of chain galaxies. , keywords =. doi:10.1051/0004-6361:20079250 , archivePrefix =. 0803.3831 , primaryClass =

    doi arXiv

  8. [16]

    , keywords =

    Modeling CO emission from hydrodynamic simulations of nearby spirals, starbursting mergers, and high-redshift galaxies. , keywords =. doi:10.1051/0004-6361/201425078 , archivePrefix =. 1409.8157 , primaryClass =

    doi arXiv

  9. [17]

    , keywords =

    The Long Lives of Giant Clumps and the Birth of Outflows in Gas-rich Galaxies at High Redshift. , keywords =. doi:10.1088/0004-637X/780/1/57 , archivePrefix =. 1307.7136 , primaryClass =

    doi arXiv

  10. [18]

    astropy/photutils: 2.0.2 , month = oct, year = 2024, publisher =

    Larry Bradley and Brigitta Sip. astropy/photutils: 2.0.2 , month = oct, year = 2024, publisher =. doi:10.5281/zenodo.13989456 , url =

    2024 doi

  11. [19]

    , keywords =

    The Mass Assembly Histories of Galaxies of Various Morphologies in the GOODS Fields. , keywords =. doi:10.1086/429549 , archivePrefix =. astro-ph/0502204 , primaryClass =

    doi arXiv

  12. [20]

    , keywords =

    High-redshift clumpy discs and bulges in cosmological simulations. , keywords =. doi:10.1111/j.1365-2966.2010.16433.x , archivePrefix =. 0907.3271 , primaryClass =

    2010 doi

  13. [21]

    , keywords =

    Radiative feedback and the low efficiency of galaxy formation in low-mass haloes at high redshift. , keywords =. doi:10.1093/mnras/stu956 , archivePrefix =. 1307.0943 , primaryClass =

    doi arXiv

  14. [22]

    , keywords =

    The Evolution of Galaxy Structure Over Cosmic Time. , keywords =. doi:10.1146/annurev-astro-081913-040037 , archivePrefix =. 1403.2783 , primaryClass =

    doi arXiv

  15. [23]

    Research Notes of the American Astronomical Society , keywords =

    Ultra-diffuse Galaxies Are a Subset of Cluster Dwarf Elliptical/Spheroidal Galaxies. Research Notes of the American Astronomical Society , keywords =. doi:10.3847/2515-5172/aab7f6 , archivePrefix =. 1803.06927 , primaryClass =

    doi arXiv

  16. [24]

    Multiwavelength Study of Massive Galaxies at z -0.5ex 2. I. Star Formation and Galaxy Growth. , keywords =. doi:10.1086/521818 , archivePrefix =. 0705.2831 , primaryClass =

    doi arXiv

  17. [25]

    , keywords =

    A Critical Assessment of Photometric Redshift Methods: A CANDELS Investigation. , keywords =. doi:10.1088/0004-637X/775/2/93 , archivePrefix =. 1308.5353 , primaryClass =

    doi arXiv

  18. [26]

    , keywords =

    The Evolution of the Specific Star Formation Rate of Massive Galaxies to z -0.5ex 1.8 in the Extended Chandra Deep Field South. , keywords =. doi:10.1088/0004-637X/690/1/937 , archivePrefix =. 0809.1426 , primaryClass =

    doi arXiv

  19. [27]

    , keywords =

    Formation of Massive Galaxies at High Redshift: Cold Streams, Clumpy Disks, and Compact Spheroids. , keywords =. doi:10.1088/0004-637X/703/1/785 , archivePrefix =. 0901.2458 , primaryClass =

    doi arXiv

  20. [28]

    , keywords =

    Wet disc contraction to galactic blue nuggets and quenching to red nuggets. , keywords =. doi:10.1093/mnras/stt2331 , archivePrefix =. 1310.1074 , primaryClass =

    doi arXiv

  21. [29]

    Near-infrared and optical broadband surface photometry of 86 face-on disk dominated galaxies. II. A two-dimensional method to determine bulge and disk parameters. , keywords =. doi:10.48550/arXiv.astro-ph/9601002 , archivePrefix =. astro-ph/9601002 , primaryClass =

    doi arXiv

  22. [30]

    , keywords =

    The structural properties of classical bulges and discs from z 2. , keywords =. doi:10.1093/mnras/stz2421 , archivePrefix =. 1902.04089 , primaryClass =

    1902 doi

  23. [31]

    , keywords =

    On the evolution of the velocity-mass-size relations of disc-dominated galaxies over the past 10 billion years. , keywords =. doi:10.1111/j.1365-2966.2010.17555.x , archivePrefix =. 1006.3558 , primaryClass =

    2010 doi

  24. [32]

    , keywords =

    Resolved Galaxies in the Hubble Ultra Deep Field: Star Formation in Disks at High Redshift. , keywords =. doi:10.1086/511667 , archivePrefix =. astro-ph/0701121 , primaryClass =

    doi arXiv

  25. [33]

    , keywords =

    Bulge Formation by the Coalescence of Giant Clumps in Primordial Disk Galaxies. , keywords =. doi:10.1086/592190 , archivePrefix =. 0808.0716 , primaryClass =

    doi arXiv

  26. [34]

    The Cosmic Evolution Early Release Science (CEERS) Survey

  27. [35]

    CEERS Key Paper. I. An Early Look into the First 500 Myr of Galaxy Formation with JWST. , keywords =. doi:10.3847/2041-8213/acade4 , archivePrefix =. 2211.05792 , primaryClass =

    doi

  28. [36]

    , keywords =

    The Cosmic Evolution Early Release Science Survey (CEERS). , keywords =. doi:10.3847/2041-8213/adbbd3 , archivePrefix =. 2501.04085 , primaryClass =

    doi

  29. [37]

    , keywords =

    Connecting Clump Sizes in Turbulent Disk Galaxies to Instability Theory. , keywords =. doi:10.3847/2041-8213/aa6478 , archivePrefix =. 1703.00458 , primaryClass =

    doi arXiv

  30. [38]

    , keywords =

    Star-Forming Galaxies at Cosmic Noon. , keywords =. doi:10.1146/annurev-astro-032620-021910 , archivePrefix =. 2010.10171 , primaryClass =

    2010 doi

  31. [39]

    , keywords =

    Structure and Star Formation in Galaxies out to z = 3: Evidence for Surface Density Dependent Evolution and Upsizing. , keywords =. doi:10.1086/592431 , archivePrefix =. 0808.2642 , primaryClass =

    doi arXiv

  32. [40]

    , keywords =

    From Rings to Bulges: Evidence for Rapid Secular Galaxy Evolution at z -0.5ex 2 from Integral Field Spectroscopy in the SINS Survey. , keywords =. doi:10.1086/591840 , archivePrefix =. 0807.1184 , primaryClass =

    doi arXiv

  33. [41]

    , keywords =

    The Sins Survey of z -0.5ex 2 Galaxy Kinematics: Properties of the Giant Star-forming Clumps. , keywords =. doi:10.1088/0004-637X/733/2/101 , archivePrefix =. 1011.5360 , primaryClass =

    doi arXiv

  34. [42]

    , keywords =

    CANDELS: The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. , keywords =. doi:10.1088/0067-0049/197/2/35 , archivePrefix =. 1105.3753 , primaryClass =

    doi arXiv

  35. [43]

    , keywords =

    Color and Stellar Population Gradients in Passively Evolving Galaxies at z -0.5ex 2 from HST/WFC3 Deep Imaging in the Hubble Ultra Deep Field. , keywords =. doi:10.1088/0004-637X/735/1/18 , archivePrefix =. 1101.0843 , primaryClass =

    doi arXiv

  36. [44]

    , keywords =

    Multi-wavelength View of Kiloparsec-scale Clumps in Star-forming Galaxies at z -0.5ex 2. , keywords =. doi:10.1088/0004-637X/757/2/120 , archivePrefix =. 1110.3800 , primaryClass =

    doi arXiv

  37. [45]

    , keywords =

    CANDELS Multi-wavelength Catalogs: Source Detection and Photometry in the GOODS-South Field. , keywords =. doi:10.1088/0067-0049/207/2/24 , archivePrefix =. 1308.4405 , primaryClass =

    doi arXiv

  38. [46]

    Clumpy Galaxies in CANDELS. I. The Definition of UV Clumps and the Fraction of Clumpy Galaxies at 0.5 < z < 3. , keywords =. doi:10.1088/0004-637X/800/1/39 , archivePrefix =. 1410.7398 , primaryClass =

    doi arXiv

  39. [47]

    Clumpy Galaxies in CANDELS. II. Physical Properties of UV-bright Clumps at 0.5 z < 3. , keywords =. doi:10.3847/1538-4357/aaa018 , archivePrefix =. 1712.01858 , primaryClass =

    doi arXiv

  40. [48]

    , keywords =

    GEMS: Galaxy Fitting Catalogs and Testing Parametric Galaxy Fitting Codes: GALFIT and GIM2D. , keywords =. doi:10.1086/518836 , archivePrefix =. 0704.2601 , primaryClass =

    doi arXiv

  41. [49]

    , keywords =

    Kiloparsec-scale Properties of Emission-line Galaxies. , keywords =. doi:10.1088/0004-637X/797/2/108 , archivePrefix =. 1409.4791 , primaryClass =

    doi arXiv

  42. [50]

    , keywords =

    Starburst galaxies in the COSMOS field: clumpy star-formation at redshift 0 < z < 0.5. , keywords =. doi:10.1051/0004-6361/201527066 , archivePrefix =. 1604.01698 , primaryClass =

    doi arXiv

  43. [51]

    , keywords =

    Subgalactic Clumps at High Redshift: A Fragmentation Origin?. , keywords =. doi:10.1086/422179 , archivePrefix =. astro-ph/0406135 , primaryClass =

    doi arXiv

  44. [52]

    , keywords =

    Gas physics, disk fragmentation, and bulge formation in young galaxies. , keywords =. doi:10.1051/0004-6361:20034282 , archivePrefix =. astro-ph/0312139 , primaryClass =

    doi arXiv

  45. [53]

    , keywords =

    Properties of thick discs formed in clumpy galaxies. , keywords =. doi:10.1093/mnras/stu544 , archivePrefix =. 1402.5986 , primaryClass =

    doi arXiv

  46. [54]

    , keywords =

    Non-linear violent disc instability with high Toomre's Q in high-redshift clumpy disc galaxies. , keywords =. doi:10.1093/mnras/stv2793 , archivePrefix =. 1510.07695 , primaryClass =

    doi arXiv

  47. [55]

    , keywords =

    Size Stellar Mass Relation and Morphology of Quiescent Galaxies at z 3 in Public JWST Fields. , keywords =. doi:10.3847/1538-4357/ad2512 , archivePrefix =. 2307.06994 , primaryClass =

    doi

  48. [56]

    , keywords =

    The Star Formation History of Mass-selected Galaxies in the COSMOS Field. , keywords =. doi:10.1088/0004-637X/730/2/61 , archivePrefix =. 1011.6370 , primaryClass =

    doi arXiv

  49. [57]

    , keywords =

    Optimized Photometric Redshifts for the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS). , keywords =. doi:10.3847/1538-4357/ac9f12 , archivePrefix =. 2210.01140 , primaryClass =

    doi

  50. [58]

    , keywords =

    CANDELS: The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey The Hubble Space Telescope Observations, Imaging Data Products, and Mosaics. , keywords =. doi:10.1088/0067-0049/197/2/36 , archivePrefix =. 1105.3754 , primaryClass =

    doi arXiv

  51. [59]

    , keywords =

    SKYSURF-3: Testing Crowded Object Catalogs in the Hubble eXtreme Deep Field Mosaics to Study Sample Incompleteness from an Extragalactic Background Light Perspective. , keywords =. doi:10.3847/2041-8213/ac9cca , archivePrefix =. 2208.07218 , primaryClass =

    doi

  52. [60]

    , keywords =

    An Ultra-Deep Near-Infrared Spectrum of a Compact Quiescent Galaxy at z = 2.2. , keywords =. doi:10.1088/0004-637X/700/1/221 , archivePrefix =. 0905.1692 , primaryClass =

    doi arXiv

  53. [61]

    FAST: Fitting and Assessment of Synthetic Templates

  54. [62]

    , keywords =

    TFIT: A Photometry Package Using Prior Information for Mixed-Resolution Data Sets. , keywords =. doi:10.1086/523898 , adsurl =

    doi

  55. [63]

    , keywords =

    The population of giant clumps in simulated high-z galaxies: in situ and ex situ migration and survival. , keywords =. doi:10.1093/mnras/stu1340 , archivePrefix =. 1311.0013 , primaryClass =

    doi arXiv

  56. [64]

    , keywords =

    Giant clumps in simulated high- z Galaxies: properties, evolution and dependence on feedback. , keywords =. doi:10.1093/mnras/stw2358 , archivePrefix =. 1512.08791 , primaryClass =

    doi arXiv

  57. [65]

    , keywords =

    The impact of dust on the sizes of galaxies in the Epoch of Reionization. , keywords =. doi:10.1093/mnras/stac380 , archivePrefix =. 2110.12075 , primaryClass =

    doi

  58. [66]

    2024 , eprint=

    UVCANDELS: Catalogs of photometric redshifts and galaxy physical properties , author=. 2024 , eprint=

    2024

  59. [67]

    , keywords =

    IROCKS: Spatially Resolved Kinematics of z 1 Star-forming Galaxies. , keywords =. doi:10.3847/0004-637X/831/1/78 , archivePrefix =. 1608.01676 , primaryClass =

    doi arXiv

  60. [68]

    , keywords =

    A deep probe of the galaxy stellar mass functions at z 1-3 with the GOODS NICMOS Survey. , keywords =. doi:10.1111/j.1365-2966.2011.18357.x , archivePrefix =. 1101.2867 , primaryClass =

    2011 doi

  61. [69]

    , keywords =

    The Evolution of Mass-Size Relation for Lyman Break Galaxies from z = 1 to z = 7. , keywords =. doi:10.1088/2041-8205/756/1/L12 , archivePrefix =. 1207.6634 , primaryClass =

    doi arXiv

  62. [70]

    , keywords =

    COSMOS-DASH: The Evolution of the Galaxy Size-Mass Relation since z 3 from New Wide-field WFC3 Imaging Combined with CANDELS/3D-HST. , keywords =. doi:10.3847/1538-4357/ab290a , archivePrefix =. 1808.04379 , primaryClass =

    doi

  63. [71]

    , keywords =

    Extending the evolution of the stellar mass-size relation at z 2 to low stellar mass galaxies from HFF and CANDELS. , keywords =. doi:10.1093/mnras/stab1744 , archivePrefix =. 2106.07663 , primaryClass =

    doi

  64. [72]

    , keywords =

    UVCANDELS: The Role of Dust on the Stellar Mass Size Relation of Disk Galaxies at 0.5 z 3.0. , keywords =. doi:10.3847/1538-4357/ad4ede , archivePrefix =. 2405.10908 , primaryClass =

    doi

  65. [73]

    , keywords =

    Spatially Resolved H Maps and Sizes of 57 Strongly Star-forming Galaxies at z -0.5ex 1 from 3D-HST: Evidence for Rapid Inside-out Assembly of Disk Galaxies. , keywords =. doi:10.1088/2041-8205/747/2/L28 , archivePrefix =. 1202.1822 , primaryClass =

    doi arXiv

  66. [74]

    , keywords =

    The Radial Distribution of Star Formation in Galaxies at z -0.5ex 1 from the 3D-HST Survey. , keywords =. doi:10.1088/2041-8205/763/1/L16 , archivePrefix =. 1301.0320 , primaryClass =

    doi arXiv

  67. [75]

    , keywords =

    Spatially Resolved Dust Maps from Balmer Decrements in Galaxies at z -0.5ex 1.4. , keywords =. doi:10.3847/2041-8205/817/1/L9 , archivePrefix =. 1511.04443 , primaryClass =

    doi arXiv

  68. [77]

    2016 , note =

    The Astrophysical Journal , author =. 2016 , note =. doi:10.3847/0004-637X/828/1/27 , abstract =

    2016 doi

  69. [78]

    , keywords =

    Millimeter Mapping at z 1: Dust-obscured Bulge Building and Disk Growth. , keywords =. doi:10.3847/1538-4357/aaf38a , archivePrefix =. 1801.02647 , primaryClass =

    doi arXiv

  70. [79]

    , keywords =

    Early Evolution of Disk Galaxies: Formation of Bulges in Clumpy Young Galactic Disks. , keywords =. doi:10.1086/306932 , archivePrefix =. astro-ph/9806355 , primaryClass =

    doi arXiv

  71. [80]

    , keywords =

    Secondary standard stars for absolute spectrophotometry. , keywords =. doi:10.1086/160817 , adsurl =

    doi

  72. [81]

    , keywords =

    The Assembly of Diversity in the Morphologies and Stellar Populations of High-Redshift Galaxies. , keywords =. doi:10.1086/429120 , archivePrefix =. astro-ph/0501088 , primaryClass =

    doi arXiv

  73. [82]

    , keywords =

    Detailed Structural Decomposition of Galaxy Images. , keywords =. doi:10.1086/340952 , archivePrefix =. astro-ph/0204182 , primaryClass =

    doi arXiv

  74. [83]

    Detailed Decomposition of Galaxy Images. II. Beyond Axisymmetric Models. , keywords =. doi:10.1088/0004-6256/139/6/2097 , archivePrefix =. 0912.0731 , primaryClass =

    doi arXiv

  75. [84]

    , keywords =

    Spitzer View on the Evolution of Star-forming Galaxies from z = 0 to z -0.5ex 3. , keywords =. doi:10.1086/431894 , archivePrefix =. astro-ph/0505101 , primaryClass =

    doi arXiv

  76. [85]

    , keywords =

    The Stellar Mass Assembly of Galaxies from z = 0 to z = 4: Analysis of a Sample Selected in the Rest-Frame Near-Infrared with Spitzer. , keywords =. doi:10.1086/523690 , archivePrefix =. 0709.1354 , primaryClass =

    doi arXiv

  77. [86]

    2022 , note =

    The Astronomical Journal , author =. 2022 , note =. doi:10.3847/1538-3881/ac5908 , abstract =

    2022 doi

  78. [87]

    , keywords =

    The Morphological Diversities among Star-forming Galaxies at High Redshifts in the Great Observatories Origins Deep Survey. , keywords =. doi:10.1086/507016 , archivePrefix =. astro-ph/0606696 , primaryClass =

    doi arXiv

  79. [88]

    , keywords =

    Stellar Masses from the CANDELS Survey: The GOODS-South and UDS Fields. , keywords =. doi:10.1088/0004-637X/801/2/97 , archivePrefix =. 1412.5180 , primaryClass =

    doi arXiv

  80. [89]

    , keywords =

    CANDELS Multi-wavelength Catalogs: Source Identification and Photometry in the CANDELS Extended Groth Strip. , keywords =. doi:10.3847/1538-4365/aa66cb , archivePrefix =. 1703.05768 , primaryClass =

    doi arXiv

  81. [90]

    , keywords =

    DAOPHOT: A Computer Program for Crowded-Field Stellar Photometry. , keywords =. doi:10.1086/131977 , adsurl =

    doi

  82. [91]

    , keywords =

    Near-exponential surface densities as hydrostatic, non-equilibrium profiles in galaxy discs. , keywords =. doi:10.1093/mnras/stw2462 , archivePrefix =. 1609.08957 , primaryClass =

    doi arXiv

  83. [92]

    , keywords =

    The Ultraviolet Luminosity Function at 0.6 < z < 1 from UVCANDELS. , keywords =. doi:10.3847/1538-4357/ad5540 , archivePrefix =. 2311.15664 , primaryClass =

    doi

  84. [93]

    , keywords =

    UVUDF: Ultraviolet Imaging of the Hubble Ultra Deep Field with Wide-Field Camera 3. , keywords =. doi:10.1088/0004-6256/146/6/159 , archivePrefix =. 1305.1357 , primaryClass =

    doi arXiv

  85. [94]

    , keywords =

    3D-HST+CANDELS: The Evolution of the Galaxy Size-Mass Distribution since z = 3. , keywords =. doi:10.1088/0004-637X/788/1/28 , archivePrefix =. 1404.2844 , primaryClass =

    doi arXiv

  86. [95]

    , keywords =

    First Results from the 3D-HST Survey: The Striking Diversity of Massive Galaxies at z > 1. , keywords =. doi:10.1088/2041-8205/743/1/L15 , archivePrefix =. 1108.6060 , primaryClass =

    doi arXiv

  87. [96]

    2017 , pages =

    Monthly Notices of the Royal Astronomical Society , author =. 2017 , pages =. doi:10.1093/mnras/stx1148 , abstract =

    2017 doi

  88. [97]

    Research Notes of the American Astronomical Society , keywords =

    Ultraviolet and Blue Optical Imaging of UVCANDELS. Research Notes of the American Astronomical Society , keywords =. doi:10.3847/2515-5172/ad1f6f , adsurl =

    doi

  89. [98]

    , keywords =

    Evolution of the Size Mass Relation of Star-forming Galaxies Since z = 5.5 Revealed by CEERS. , keywords =. doi:10.3847/1538-4357/ad20ed , archivePrefix =. 2311.02162 , primaryClass =

    doi

  90. [99]

    , keywords =

    The Star Formation Mass Sequence Out to z = 2.5. , keywords =. doi:10.1088/2041-8205/754/2/L29 , archivePrefix =. 1205.0547 , primaryClass =

    doi arXiv

  91. [100]

    Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results

    JWST PEARLS. Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results. , keywords =. doi:10.3847/1538-3881/aca163 , archivePrefix =. 2209.04119 , primaryClass =

    doi

  92. [101]

    , keywords =

    The KMOS ^ 3D Survey: Data Release and Final Survey Paper. , keywords =. doi:10.3847/1538-4357/ab4db8 , archivePrefix =. 1909.11096 , primaryClass =

    1909 doi

  93. [102]

    , keywords =

    Photometric properties of reionization-epoch galaxies in the SIMBA simulations. , keywords =. doi:10.1093/mnras/staa1044 , archivePrefix =. 1911.06330 , primaryClass =

    1911 doi

  94. [103]

    , keywords =

    A CANDELS-3D-HST synergy: Resolved Star Formation Patterns at 0.7 < z < 1.5. , keywords =. doi:10.1088/0004-637X/779/2/135 , archivePrefix =. 1310.5702 , primaryClass =

    doi arXiv

  95. [104]

    , keywords =

    Smooth(er) Stellar Mass Maps in CANDELS: Constraints on the Longevity of Clumps in High-redshift Star-forming Galaxies. , keywords =. doi:10.1088/0004-637X/753/2/114 , archivePrefix =. 1203.2611 , primaryClass =

    doi arXiv

  96. [105]

    , keywords =

    Galaxy Structure and Mode of Star Formation in the SFR-Mass Plane from z -0.5ex 2.5 to z -0.5ex 0.1. , keywords =. doi:10.1088/0004-637X/742/2/96 , archivePrefix =. 1107.0317 , primaryClass =

    doi arXiv

  97. [106]

    , keywords =

    On Star Formation Rates and Star Formation Histories of Galaxies Out to z -0.5ex 3. , keywords =. doi:10.1088/0004-637X/738/1/106 , archivePrefix =. 1106.5502 , primaryClass =

    doi arXiv

  98. [107]

    , keywords =

    An extremely young massive clump forming by gravitational collapse in a primordial galaxy. , keywords =. doi:10.1038/nature14409 , archivePrefix =. 1505.01290 , primaryClass =

    doi arXiv

Pith tools

Reviewed June 26, 2026 · model on record in the stance chip above.