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arxiv: 2605.15361 · v1 · pith:HUSCQSV5new · submitted 2026-05-14 · 🌌 astro-ph.GA

Clumps in spiral galaxies at z lesssim 3: Disentangling two spatial modes of star formation

Ilia V. Chugunov , Alexander A. Marchuk This is my paper

Pith reviewed 2026-05-19 15:06 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords spiral galaxiesstar-forming clumpshigh-redshift galaxiesphotometric modelingresidual imagesstar formation modesHST JWST observations
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The pith

Spiral arms stimulate clump formation in galaxies out to redshift 3.3 without changing the clumps' star formation properties.

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

The paper analyzes 159 spiral galaxies from z=0.1 to 3.3 using HST and JWST images. It identifies 3003 clumps in residual images after separate photometric modeling of spiral arms. Clumps turn out smaller in luminosity, mass and size than earlier studies reported, and they concentrate spatially toward the arms with correlated parameters. Clumps inside arms are smaller yet brighter than inter-arm clumps, while their colors remain similar. This points to arms acting as a trigger for clumps while leaving the underlying star formation process unchanged.

Core claim

Using residual images from photometric models that include spiral arms yields clumps whose luminosities, masses and sizes are smaller than commonly accepted. Clumps concentrate toward spiral arms, their parameters correlate with arm properties, and arm clumps are smaller but brighter than inter-arm clumps while sharing similar colors. The results indicate that spiral arms stimulate clump formation although the star formation properties of the clumps themselves remain unchanged compared to the inter-arm region.

What carries the argument

Residual images obtained after subtracting photometric models that separately fit spiral arms, which permit clean identification and measurement of clumps apart from arm light.

If this is right

  • Clumps inside spiral arms are smaller yet brighter than those in inter-arm regions.
  • Clump and spiral parameters show measurable correlations.
  • Colors and other star-formation indicators remain similar for clumps in and out of arms.
  • Clumps in modeled spiral galaxies have lower luminosities, masses and sizes than values reported for clumpy galaxies without arm modeling.

Where Pith is reading between the lines

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

  • Applying the same arm-subtraction method to galaxies at still higher redshifts could test whether the stimulation effect strengthens or weakens with look-back time.
  • Many galaxies previously classified as clumpy may contain undetected spiral structure revealed only after arm modeling.
  • The unchanged colors suggest the arm trigger acts through increased gas density or dynamical compression rather than by changing the initial mass function inside the clumps.

Load-bearing premise

The photometric models that include spiral arms produce residuals in which clumps can be cleanly identified and measured without significant artifacts or over-subtraction from the arm modeling process.

What would settle it

A re-analysis of the same images using alternative spiral-arm models that yields substantially different clump counts, sizes or spatial distributions would falsify the claim that arms stimulate clump formation.

Figures

Figures reproduced from arXiv: 2605.15361 by Alexander A. Marchuk, Ilia V. Chugunov.

Figure 1
Figure 1. Figure 1: A schematic diagram showing the main steps in clumps’ detection and parameters measurement. Top left: an example image of a galaxy from our sample. Top right: photometric model with spiral arms from Paper I. Middle left: residual image from Paper I (image minus model), where orange represents positive values (model underestimates image), purple is negative and white is zero. Middle right: segmentation imag… view at source ↗
Figure 2
Figure 2. Figure 2: A collage showing an example galaxy image (rightmost) and its models (three remaining columns). Top row shows original models. Bottom row shows the same models with superimposed noise of the same magnitude as in original image for visual comparison with it. From left to right: a classical model (bulge + disc) from Paper I, a model including spiral arms from Paper I and a model with spiral arms with added c… view at source ↗
Figure 3
Figure 3. Figure 3: An example of SED fitting result using Prospector. Observed fluxes are shown in squares, each one corresponds to a single filter; their passbands are shown in bottom. The model spectrum is shown as a thin curve, and corresponding model photometry is represented by circles. The parameters of the fit (see Conroy & Gunn 2010; Johnson et al. 2021) are shown in the legend. MNRAS 000, 1–20 (2026) [PITH_FULL_IMA… view at source ↗
Figure 4
Figure 4. Figure 4: The dependence of total clumps count in a galaxy 𝑁𝑐 on look￾back time 𝑡𝐿. Black squares with error bars represent binned averages, with horizontal bars representing bin ranges and vertical standing for standard deviations. 3 RESULTS After we applied our method of clumps identification and measured their parameters, we found a total of 3003 clumps, or 19 per galaxy on average. Only 4 galaxies out of 159 hav… view at source ↗
Figure 6
Figure 6. Figure 6: we show how 𝐶/𝑇 and 𝑁𝑐 changes for individual galaxies with artificial redshifting. It is seen that decreasing image quality mostly decreases observed 𝐶/𝑇 as well as the number of detected clumps. In distant galaxies, faint features are more likely to remain undetected, and tight groups of clumps can appear as a single object. However, this conclusion is qualitative, and we will account for varying image q… view at source ↗
Figure 5
Figure 5. Figure 5: Top: the dependence of clump-to-total ratio 𝐶/𝑇 on rest-frame wavelength 𝜆rf for individual galaxies from JWST subsample. Bottom: 𝐶/𝑇 normalised to the same level (corresponding to a unity for rest-frame wave￾length of 𝐹814𝑊 filter) for different galaxies. Normalization is done by fitting the same square logarithmic function (shown as a thick line) with normalisation coefficients individual for each galaxy… view at source ↗
Figure 7
Figure 7. Figure 7: Left: clump-to-total ratio 𝐶/𝑇 versus lookback time 𝑡𝐿 for individual galaxies. Middle: the same, for clump-to-total ratio corrected to represent the F814W filter, 𝐶/𝑇F814W. Right: the fraction of galaxies with 𝐶/𝑇F814W > 0.04 in the same bins. Here, vertical error bars represent the 95% confidence intervals. any case, our findings apply only to spiral galaxies which also may influence results. Regarding i… view at source ↗
Figure 8
Figure 8. Figure 8: The dependence of 𝐶/𝑇F814W on three parameters. From left to right: lookback time 𝑡𝐿 (limited to 𝑡𝐿 < 9 Gyr), absolute magnitude of the host galaxy 𝑀F814W and signal-to-noise ratio of a galaxy lg SNR. Red line shows the projections of a trilinear function fitted jointly to 𝐶/𝑇F814W depending on all three parameters, to each single parameter. For comparison, green dashed line shows a single linear fit to 𝐶/… view at source ↗
Figure 10
Figure 10. Figure 10: A diagram showing the comparison between 𝐶/𝑇 of galaxies from JWST samples, measured with different methods: the one from our work, and another from Kalita et al. (2025a). 1:1 line is shown, as well as average values. luminous clumps, its spiral structure becomes difficult to be recog￾nized, and it is not included in our sample of spiral galaxies. There is no statistically significant correlation between … view at source ↗
Figure 12
Figure 12. Figure 12: A stacked histogram of logarithm of effective radii 𝑟𝑒 for individual clumps. Red shaded area on the left represents 𝑟𝑒 < 270 pc, which is the typical size of PSF, so their exact measurements are not highly reliable. and have average 𝑧 = 1.5) yields the median clump size of 360 pc. The reasons for this difference can possibly be similar to those for clump luminosities (see discussion in Section 3.1). Firs… view at source ↗
Figure 13
Figure 13. Figure 13: Clumps 𝑟𝑒 versus their absolute magnitude 𝑀F814W. Lines of constant average surface brightness are also shown: from left to right, they correspond to 10, 100 and 1000 𝐿⊙/pc2 . Effectively unresolved clumps (𝑟𝑒 < 270 pc) are not shown [PITH_FULL_IMAGE:figures/full_fig_p011_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: The distributions of galactocentric distance 𝑟𝑐 of individual clumps, normalised to disc exponential scale ℎ. Left: a stacked histogram of 𝑟𝑐/ℎ for individual clumps. Right: a stacked histogram of ⟨𝑟𝑐/ℎ⟩ for individ￾ual galaxies in our sample, i.e. 𝑟𝑐/ℎ averaged over entire galaxy (weighted average by clump luminosity was used). Green shaded area represents the range of galactocentric radii where spiral c… view at source ↗
Figure 16
Figure 16. Figure 16: Top: a stacked histogram of the fraction of clumps located in spiral arms 𝑓cs(0.2) for individual galaxies with at least 5 detected clumps. Here, spiral mask is defined as 20% disc pixels with highest brightness of spirals. Bottom: the heat map showing the distributions of 𝑓cs(𝑥) for different 𝑥 (each column represents a histogram for single 𝑥). Average 𝑓cs(𝑥) values are also shown. Cyan circles show true… view at source ↗
Figure 17
Figure 17. Figure 17: Diagrams of clumps concentration towards spirals 𝑓cs(0.2) de￾pendence on different parameters of a galaxy. Top left: spiral-to-total ratio 𝑆/𝑇. Top right: asymmetry index of the spiral structure 𝐴sp for two-armed spirals. Bottom left: clump-to-total ratio 𝐶/𝑇F814W. Bottom right: bulge-to￾total ratio 𝐵/𝑇. In the legend, Pearson correlation coefficient and p-value are shown. 3.5.1 Colour indices Colour inde… view at source ↗
Figure 18
Figure 18. Figure 18: The relations between approximate colour (𝑔 − 𝑟 )app of clumps and different parameters of a galaxy. Left: colour (𝑔 − 𝑟 )app of the disc. Middle: colour (𝑔 − 𝑟 )app of spiral structure. Right: absolute magnitude of a galaxy 𝑀F814W. Dashed lines represent 1:1 relation. Solid lines show linear fits [PITH_FULL_IMAGE:figures/full_fig_p014_18.png] view at source ↗
Figure 20
Figure 20. Figure 20: Left: diagram showing the relation between stellar mass-to-light ratio 𝛾 F814W and approximate colour index (𝑔 − 𝑟 )app for clumps with good quality SED fitting. The linear fit (colour–stellar mass-to-light ratio, CMLR) is shown, as well as 𝑖 and 𝑧-band CMLR for local galaxies from Roediger & Courteau (2015). Right: a stacked histogram showing the distribution of clumps by mass. For small number, it is de… view at source ↗
Figure 21
Figure 21. Figure 21: Histograms showing clumps distributions by different parameters, with clumps in spirals and clumps in inter-arm region are separated. For absolute magnitude 𝑀F814W (top left) and effective radius 𝑟𝑒 (bottom left), the data is binned by lookback time 𝑡𝐿. Colour (𝑔 − 𝑟 )app, mass 𝑀∗ and age 𝑡 (three boxes on top right) are not binned and only available for JWST subsample, at 𝑧 > 1. Each histogram is two-sid… view at source ↗
read the original abstract

At high redshifts, star formation in galaxies is more often concentrated in clumps than in spiral arms. Although clumps are actively studied, it is rarely done considering spiral arms as objects for study as well, and the connection between clumps and spirals remains understudied. We used a sample of 159 spiral galaxies at $0.1 \leq z \leq 3.3$ observed by HST and JWST. Using the residual images from photometric models with spiral arms constructed before, which was not done previously, we have done identification of clumps and measured their properties with photometric decomposition, finding 3003 clumps in overall, and performing SED fitting for a fraction of them. We examined the overall properties of clumps, focusing on the properties of spiral structure. We found that clumps luminosities, masses and sizes are smaller than commonly accepted in literature, either for the reason spiral arms were modelled separately, or because clumps in spiral galaxies are different compared to clumpy ones. We demonstrate the connection between clumps and spirals, in particular clumps are spatially concentrated towards spirals and various parameters of clumps and spirals correlate. Also, clumps in spiral arms tend to be smaller but brighter compared to clumps in inter-arm area, but their colours are similar. There are also some differences between clumps and spirals such as colour, emphasizing the importance of their separate analysis. Our results probably indicate that spiral arms stimulate the formation of clumps, although star formation properties of clumps in spiral arms is not changed compared to inter-arm region.

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 / 3 minor

Summary. The manuscript analyzes clumps in a sample of 159 spiral galaxies at 0.1 ≤ z ≤ 3.3 observed with HST and JWST. By constructing photometric models that explicitly include spiral arms and working with the resulting residual images (an approach not previously applied), the authors identify and photometrically decompose 3003 clumps, perform SED fitting on a subset, and compare clump properties inside versus outside spiral arms. They report that clumps are smaller, less luminous, and less massive than values commonly cited in the literature; that clumps are spatially concentrated toward spiral arms; that arm clumps are smaller but brighter than inter-arm clumps while sharing similar colors; and that various clump and spiral parameters correlate. The authors conclude that spiral arms stimulate clump formation without altering the underlying star-formation properties relative to inter-arm regions.

Significance. If the central results hold after addressing methodological concerns, the work would be significant for disentangling two spatial modes of star formation and for demonstrating a direct connection between spiral structure and clump formation across a wide redshift range. The large sample, the explicit arm modeling step, and the reported differences in clump size/brightness between arm and inter-arm environments could help reconcile discrepancies in the clump literature and motivate new theoretical work on how density waves influence clump formation.

major comments (2)
  1. [Methods / residual-image analysis] The central claim that spiral arms stimulate clump formation rests on the spatial concentration and property differences measured in residuals after spiral-arm photometric modeling. No quantitative validation (e.g., injection-recovery tests or direct comparison of clump catalogs derived with versus without arm modeling) is described to demonstrate that residuals are free of systematic subtraction artifacts at the clump scale; such artifacts could artificially enhance the apparent arm-clump correlation.
  2. [Results / clump properties and correlations] The abstract reports a sample of 159 galaxies and 3003 clumps plus SED fitting on a fraction, but provides no error bars on derived quantities, no explicit criteria for data exclusion or model assumptions, and no quantitative measures (e.g., correlation coefficients or significance levels) of the claimed clump-spiral parameter correlations. These omissions leave the strength of the reported trends difficult to assess.
minor comments (3)
  1. [Title and abstract] The title states z ≲ 3 while the abstract gives 0.1 ≤ z ≤ 3.3; ensure consistency or clarify the exact upper limit.
  2. [Abstract / methods] Specify the exact number (or fraction) of clumps for which SED fitting was performed and the fitting code, templates, and priors used.
  3. [Results] Clarify whether the reported size, luminosity, and mass differences between arm and inter-arm clumps are statistically significant after accounting for selection effects and measurement uncertainties.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive feedback on our manuscript. We address each major comment below and describe the revisions we will implement to strengthen the paper.

read point-by-point responses

  1. Referee: [Methods / residual-image analysis] The central claim that spiral arms stimulate clump formation rests on the spatial concentration and property differences measured in residuals after spiral-arm photometric modeling. No quantitative validation (e.g., injection-recovery tests or direct comparison of clump catalogs derived with versus without arm modeling) is described to demonstrate that residuals are free of systematic subtraction artifacts at the clump scale; such artifacts could artificially enhance the apparent arm-clump correlation.

    Authors: We agree that explicit quantitative validation would increase confidence in the residual-based clump catalog. The spiral-arm modeling follows standard photometric decomposition techniques previously validated on lower-redshift samples, and residuals were inspected to remove obvious artifacts before clump detection. However, the original submission did not include injection-recovery tests or side-by-side catalog comparisons. In the revised manuscript we will add injection-recovery experiments: simulated clumps of varying size, brightness, and position will be inserted into the original images, the full arm-modeling and residual pipeline will be re-run, and recovery fractions plus any systematic biases in arm versus inter-arm regions will be reported. This directly quantifies potential subtraction artifacts at the clump scale. revision: yes

  2. Referee: [Results / clump properties and correlations] The abstract reports a sample of 159 galaxies and 3003 clumps plus SED fitting on a fraction, but provides no error bars on derived quantities, no explicit criteria for data exclusion or model assumptions, and no quantitative measures (e.g., correlation coefficients or significance levels) of the claimed clump-spiral parameter correlations. These omissions leave the strength of the reported trends difficult to assess.

    Authors: We accept that the presentation of statistical details can be improved for clarity. While the methods section describes the fitting procedures and sample selection, error bars, exclusion criteria, and quantitative correlation statistics were not uniformly reported. In the revision we will (i) attach uncertainties to all reported clump sizes, luminosities, and masses, (ii) explicitly list the data-exclusion criteria (e.g., signal-to-noise thresholds, convergence criteria for fits) and model assumptions (e.g., functional forms for arms and clumps), and (iii) provide Spearman or Pearson correlation coefficients together with their p-values for every claimed clump-spiral parameter correlation. revision: yes

Circularity Check

0 steps flagged

No significant circularity; results derive from direct observational measurements

full rationale

The paper's derivation chain consists of applying photometric decomposition to residual images after spiral-arm modeling, identifying 3003 clumps, and reporting spatial correlations and property differences between arm and inter-arm regions. No equations, fitted parameters, or predictions are presented that reduce by construction to the input data or to self-citations. The use of prior arm models is described as a novel application rather than a load-bearing uniqueness theorem imported from the authors' own work. The central claims remain independent of any definitional loop or renamed empirical pattern.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Based on abstract only; no explicit free parameters, axioms, or invented entities are described.

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Works this paper leans on

160 extracted references · 160 canonical work pages · 7 internal anchors

  1. [1]

    Adams, Dominic and Mehta, Vihang and Dickinson, Hugh and Scarlata, Claudia and Fortson, Lucy and Kruk, Sandor and Simmons, Brooke and Lintott, Chris , year =. Galaxy. The Astrophysical Journal , volume =. doi:10.3847/1538-4357/ac6512 , keywords =

    work page doi:10.3847/1538-4357/ac6512

  2. [2]

    and Finkelstein, Steven L

    Bagley, Micaela B. and Finkelstein, Steven L. and Koekemoer, Anton M. and Ferguson, Henry C. and Arrabal Haro, Pablo and Dickinson, Mark and Kartaltepe, Jeyhan S. and Papovich, Casey and. 2023 , month = mar, journal =. doi:10.3847/2041-8213/acbb08 , keywords =

    work page doi:10.3847/2041-8213/acbb08 2023

  3. [3]

    and Wisnioski, Emily and Damjanov, Ivana and Abraham, Roberto and Obreschkow, Danail and Green, Andrew W

    Bassett, Robert and Glazebrook, Karl and Fisher, David B. and Wisnioski, Emily and Damjanov, Ivana and Abraham, Roberto and Obreschkow, Danail and Green, Andrew W. and. Integrated and Resolved Dust Attenuation in Clumpy Star-Forming Galaxies at 0.07. 2017 , month = may, journal =. doi:10.1093/mnras/stw2983 , keywords =

    work page doi:10.1093/mnras/stw2983 2017

  4. [4]

    Battisti, A. J. and. Avoiding (Photo-z). 2025 , month = jul, journal =. doi:10.3847/2515-5172/adea37 , keywords =

    work page doi:10.3847/2515-5172/adea37 2025

  5. [5]

    , year =

    Bekki, K. , year =. Quantifying the Fine Structures of Disk Galaxies with Deep Learning:. Astronomy and Astrophysics , volume =. doi:10.1051/0004-6361/202039797 , keywords =

    work page doi:10.1051/0004-6361/202039797

  6. [6]

    and Zhou, YanYan , year =

    Berger, Vance W. and Zhou, YanYan , year =. Kolmogorov--. Wiley. doi:10.1002/9781118445112.stat06558 , copyright =

    work page doi:10.1002/9781118445112.stat06558

  7. [7]

    Galactic

    Binney, James and Tremaine, Scott , year = 2008, month = jan, journal =. Galactic

    work page 2008

  8. [8]

    Larry Bradley and Brigitta Sipőcz and Thomas Robitaille and Erik Tollerud and Zé Vinícius and Christoph Deil and Kyle Barbary and Tom J Wilson and Ivo Busko and Axel Donath and Hans Moritz Günther and Mihai Cara and P. L. Lim and Sebastian Meßlinger and Zach Burnett and Simon Conseil and Michael Droettboom and Azalee Bostroem and E. M. Bray and Lars Ander...

    work page doi:10.5281/zenodo.12585239

  9. [9]

    Brooks, Alyson and Christensen, Charlotte , year =. Bulge. Galactic. doi:10.1007/978-3-319-19378-6_12 , keywords =

    work page doi:10.1007/978-3-319-19378-6_12

  10. [10]

    2021 , month = dec, journal =

    Radii of Young Star Clusters in Nearby Galaxies , author =. 2021 , month = dec, journal =. doi:10.1093/mnras/stab2907 , keywords =

    work page doi:10.1093/mnras/stab2907 2021

  11. [11]

    2017 , month = jul, journal =

    Buck, Tobias and Macci. 2017 , month = jul, journal =. doi:10.1093/mnras/stx685 , keywords =

    work page doi:10.1093/mnras/stx685 2017

  12. [12]

    Recovering the Origins of the Lenticular Galaxy

    Buzzo, Maria Luisa and Cortesi, Arianna and. Recovering the Origins of the Lenticular Galaxy. 2021 , month = jun, journal =. doi:10.1093/mnras/stab941 , keywords =

    work page doi:10.1093/mnras/stab941 2021

  13. [13]

    A solar-metallicity and dusty DLA at z _ abs = 2.58

    Cacciato, Marcello and Dekel, Avishai and Genel, Shy , year =. Evolution of Violent Gravitational Disc Instability in Galaxies: Late Stabilization by Transition from Gas to Stellar Dominance , shorttitle =. Monthly Notices of the Royal Astronomical Society , volume =. doi:10.1111/j.1365-2966.2011.20359.x , keywords =

    work page doi:10.1111/j.1365-2966.2011.20359.x 2011

  14. [14]

    2019 , month = dec, journal =

    Merger Induced Clump Formation in Distant Infrared Luminous Starburst Galaxies , author =. 2019 , month = dec, journal =. doi:10.1051/0004-6361/201935778 , keywords =

    work page doi:10.1051/0004-6361/201935778 2019

  15. [15]

    and Stiavelli, M

    Calvi, V. and Stiavelli, M. and Bradley, L. and Pizzella, A. and Kim, S. , year =. The. The Astrophysical Journal , volume =. doi:10.1088/0004-637X/796/2/102 , keywords =

    work page doi:10.1088/0004-637x/796/2/102

  16. [16]

    Carilli, C. L. and Walter, F. , year =. Cool. Annual Review of Astronomy and Astrophysics , volume =. doi:10.1146/annurev-astro-082812-140953 , keywords =

    work page doi:10.1146/annurev-astro-082812-140953

  17. [17]

    and Maiolino, R

    Carniani, S. and Maiolino, R. and Pallottini, A. and Vallini, L. and Pentericci, L. and Ferrara, A. and Castellano, M. and Vanzella, E. and Grazian, A. and Gallerani, S. and Santini, P. and Wagg, J. and Fontana, A. , year =. Extended Ionised and Clumpy Gas in a Normal Galaxy at z = 7.1 Revealed by. Astronomy and Astrophysics , volume =. doi:10.1051/0004-6...

    work page doi:10.1051/0004-6361/201630366

  18. [18]

    2018 , month = nov, journal =

    The Nature of Giant Clumps in Distant Galaxies Probed by the Anatomy of the Cosmic Snake , author =. 2018 , month = nov, journal =. doi:10.1038/s41550-017-0295-x , keywords =

    work page doi:10.1038/s41550-017-0295-x 2018

  19. [19]

    and Marchuk, Alexander A

    Chugunov, Ilia V. and Marchuk, Alexander A. and Mosenkov, Aleksandr V. and Savchenko, Sergey S. and Shishkina, Ekaterina V. and Chazov, Maxim I. and Nazarova, Aleksandra E. and Skryabina, Maria N. and Smirnova, Polina I. and Smirnov, Anton A. , year =. Galaxies Decomposition with Spiral Arms -. Monthly Notices of the Royal Astronomical Society , volume =....

    work page doi:10.1093/mnras/stad3850

  20. [20]

    and Marchuk, Alexander A

    Chugunov, Ilia V. and Marchuk, Alexander A. and Mosenkov, Aleksandr V. , year =. Less Wound and More Asymmetric:. Publications of the Astronomical Society of Australia , volume =. doi:10.1017/pasa.2025.6 , keywords =

    work page doi:10.1017/pasa.2025.6 2025

  21. [21]

    and Marchuk, Alexander A

    Chugunov, Ilia V. and Marchuk, Alexander A. and Savchenko, Sergey S. , year =. Examination of the. Galaxies , volume =. doi:10.3390/galaxies13020044 , copyright =

    work page doi:10.3390/galaxies13020044

  22. [22]

    and Daddi, E

    Cibinel, A. and Daddi, E. and Bournaud, F. and Sargent, M. T. and. 2017 , month = aug, journal =. doi:10.1093/mnras/stx1112 , keywords =

    work page doi:10.1093/mnras/stx1112 2017

  23. [23]

    Star Formation at the Smallest Scales: A

    Claeyssens, Ad. Star Formation at the Smallest Scales: A. 2023 , month = apr, journal =. doi:10.1093/mnras/stac3791 , keywords =

    work page doi:10.1093/mnras/stac3791 2023

  24. [24]

    Tracing Star Formation across Cosmic Time at Tens of Parsec-Scales in the Lensing Cluster Field

    Claeyssens, Ad. Tracing Star Formation across Cosmic Time at Tens of Parsec-Scales in the Lensing Cluster Field. 2025 , month = mar, journal =. doi:10.1093/mnras/staf058 , keywords =

    work page doi:10.1093/mnras/staf058 2025

  25. [25]

    Clark, C. J. R. and Verstocken, S. and Bianchi, S. and Fritz, J. and Viaene, S. and Smith, M. W. L. and Baes, M. and Casasola, V. and Cassara, L. P. and Davies, J. I. and De Looze, I. and De Vis, P. and Evans, R. and Galametz, M. and Jones, A. P. and Lianou, S. and Madden, S. and Mosenkov, A. V. and Xilouris, M. , year = 2018, month = jan, journal =. doi:...

    work page doi:10.1051/0004-6361/201731419 2018

  26. [26]

    , year =

    Conroy, Charlie and Gunn, James E. , year =. Astrophysics Source Code Library , pages =

    work page

  27. [27]

    Modeling the

    Conroy, Charlie , year =. Modeling the. Annual Review of Astronomy and Astrophysics , volume =. doi:10.1146/annurev-astro-082812-141017 , keywords =

    work page internal anchor Pith review doi:10.1146/annurev-astro-082812-141017

  28. [28]

    , eprint =

    The Fundamental Properties of Galaxies and a New Galaxy Classification System , author =. 2006 , month = dec, journal =. doi:10.1111/j.1365-2966.2006.11114.x , keywords =

    work page doi:10.1111/j.1365-2966.2006.11114.x 2006

  29. [29]

    , year =

    Conselice, Christopher J. , year =. The. Annual Review of Astronomy and Astrophysics , volume =. doi:10.1146/annurev-astro-081913-040037 , keywords =

    work page doi:10.1146/annurev-astro-081913-040037

  30. [30]

    and Mundy, Carl J

    Conselice, Christopher J. and Mundy, Carl J. and Ferreira, Leonardo and Duncan, Kenneth , year =. A. The Astrophysical Journal , volume =. doi:10.3847/1538-4357/ac9b1a , keywords =

    work page doi:10.3847/1538-4357/ac9b1a

  31. [31]

    and Hayes, Wayne B

    Davis, Darren R. and Hayes, Wayne B. , year =. The Astrophysical Journal , volume =. doi:10.1088/0004-637X/790/2/87 , keywords =

    work page doi:10.1088/0004-637x/790/2/87

  32. [32]

    Formation of

    Dekel, Avishai and Sari, Re'em and Ceverino, Daniel , year =. Formation of. The Astrophysical Journal , volume =. doi:10.1088/0004-637X/703/1/785 , keywords =

    work page doi:10.1088/0004-637x/703/1/785

  33. [33]

    and Ginzburg, Omri and Mandelker, Nir and Ceverino, Daniel and Primack, Joel , year =

    Dekel, Avishai and Tziperman, Offek and Sarkar, Kartick C. and Ginzburg, Omri and Mandelker, Nir and Ceverino, Daniel and Primack, Joel , year =. Conditions for Clump Survival in. Monthly Notices of the Royal Astronomical Society , volume =. doi:10.1093/mnras/stad855 , keywords =

    work page doi:10.1093/mnras/stad855

  34. [34]

    The Fraction of Clumpy Galaxies in JADES over $2<z<9$

    The. 2025 , month = aug, publisher =. doi:10.48550/arXiv.2508.14972 , keywords =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2508.14972 2025

  35. [35]

    2017 , month = feb, journal =

    On the. 2017 , month = feb, journal =. doi:10.3847/2041-8213/aa5d52 , keywords =

    work page doi:10.3847/2041-8213/aa5d52 2017

  36. [36]

    2023 , month = mar, journal =

    Molecular Gas Cloud Properties at z. 2023 , month = mar, journal =. doi:10.1093/mnras/stad113 , keywords =

    work page doi:10.1093/mnras/stad113 2023

  37. [37]

    Dobbs, Clare and Baba, Junichi , year =. Dawes. Publications of the Astronomical Society of Australia , volume =. doi:10.1017/pasa.2014.31 , keywords =

    work page doi:10.1017/pasa.2014.31 2014

  38. [38]

    , year =

    Dressler, A. , year =. Galaxy Morphology in Rich Clusters: Implications for the Formation and Evolution of Galaxies. , shorttitle =. The Astrophysical Journal , volume =. doi:10.1086/157753 , keywords =

    work page doi:10.1086/157753

  39. [39]

    , year =

    Du, Wei and McGaugh, Stacy S. , year =. Self-Consistent. The Astronomical Journal , volume =. doi:10.3847/1538-3881/aba754 , keywords =

    work page doi:10.3847/1538-3881/aba754

  40. [40]

    Overview of the JWST Advanced Deep Extragalactic Survey (JADES)

    Eisenstein, Daniel J. and Willott, Chris and Alberts, Stacey and Arribas, Santiago and Bonaventura, Nina and Bunker, Andrew J. and Cameron, Alex J. and Carniani, Stefano and Charlot, Stephane and. Overview of the. 2023 , month = jun, journal =. doi:10.48550/arXiv.2306.02465 , keywords =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2306.02465 2023

  41. [41]

    and Rubin, Douglas S

    Elmegreen, Debra Meloy and Elmegreen, Bruce G. and Rubin, Douglas S. and Schaffer, Meredith A. , year =. Galaxy. The Astrophysical Journal , volume =. doi:10.1086/432502 , keywords =

    work page doi:10.1086/432502

  42. [42]

    and Ravindranath, Swara and Coe, Daniel A

    Elmegreen, Debra Meloy and Elmegreen, Bruce G. and Ravindranath, Swara and Coe, Daniel A. , year =. Resolved. The Astrophysical Journal , volume =. doi:10.1086/511667 , keywords =

    work page doi:10.1086/511667

  43. [43]

    and Bournaud, Fr

    Elmegreen, Bruce G. and Bournaud, Fr. Bulge. 2008 , month = nov, journal =. doi:10.1086/592190 , keywords =

    work page doi:10.1086/592190 2008

  44. [44]

    and Elmegreen, Debra Meloy and Fernandez, Maria Ximena and Lemonias, Jenna Jo , year =

    Elmegreen, Bruce G. and Elmegreen, Debra Meloy and Fernandez, Maria Ximena and Lemonias, Jenna Jo , year =. Bulge and. The Astrophysical Journal , volume =. doi:10.1088/0004-637X/692/1/12 , keywords =

    work page doi:10.1088/0004-637x/692/1/12

  45. [45]

    Tracing the

    Epinat, Beno. Tracing the. 2011 , month = dec, volume =. doi:10.1017/S1743921311022617 , keywords =

    work page doi:10.1017/s1743921311022617 2011

  46. [46]

    The Astrophysical Journal , volume =

    Erwin, Peter , year =. The Astrophysical Journal , volume =. doi:10.1088/0004-637X/799/2/226 , keywords =

    work page doi:10.1088/0004-637x/799/2/226

  47. [47]

    Espejo Salcedo, J. M. and Pastras, S. and V. Galaxy Morphologies at Cosmic Noon with. 2025 , month = aug, journal =. doi:10.1051/0004-6361/202554725 , keywords =

    work page doi:10.1051/0004-6361/202554725 2025

  48. [48]

    2025 , month = oct, journal =

    Metal-Poor. 2025 , month = oct, journal =. doi:10.3847/1538-4357/adfb64 , keywords =

    work page doi:10.3847/1538-4357/adfb64 2025

  49. [49]

    2014 , month = feb, journal =

    Balance among Gravitational Instability, Star Formation and Accretion Determines the Structure and Evolution of Disc Galaxies , author =. 2014 , month = feb, journal =. doi:10.1093/mnras/stt2294 , keywords =

    work page doi:10.1093/mnras/stt2294 2014

  50. [50]

    2018 , month = may, journal =

    Classifying and Modelling Spiral Structures in Hydrodynamic Simulations of Astrophysical Discs , author =. 2018 , month = may, journal =. doi:10.1093/mnras/sty331 , keywords =

    work page doi:10.1093/mnras/sty331 2018

  51. [51]

    and Rix, H.-W

    Foyle, K. and Rix, H.-W. and Walter, F. and Leroy, A. K. , year =. Arm and. The Astrophysical Journal , volume =. doi:10.1088/0004-637X/725/1/534 , keywords =

    work page doi:10.1088/0004-637x/725/1/534

  52. [52]

    Nature Astronomy , volume =

    Primordial Rotating Disk Composed of at Least 15 Dense Star-Forming Clumps at Cosmic Dawn , author =. Nature Astronomy , volume =. doi:10.1038/s41550-025-02592-w , keywords =

    work page doi:10.1038/s41550-025-02592-w

  53. [53]

    and Ichikawa, T

    Fukugita, M. and Ichikawa, T. and Gunn, J. E. and Doi, M. and Shimasaku, K. and Schneider, D. P. , year =. The. The Astronomical Journal , volume =. doi:10.1086/117915 , keywords =

    work page doi:10.1086/117915

  54. [54]

    A Grand-Design Spiral Galaxy 1.5 Billion Years after the

    Jain, Rashi and Wadadekar, Yogesh , year =. A Grand-Design Spiral Galaxy 1.5 Billion Years after the. Astronomy and Astrophysics , volume =. doi:10.1051/0004-6361/202451689 , keywords =

    work page doi:10.1051/0004-6361/202451689

  55. [55]

    and Tacconi, L

    Genzel, R. and Tacconi, L. J. and Eisenhauer, F. and F. The Rapid Formation of a Large Rotating Disk Galaxy Three Billion Years after the. 2006 , month = aug, journal =. doi:10.1038/nature05052 , keywords =

    work page doi:10.1038/nature05052 2006

  56. [56]

    and Newman, S

    Genzel, R. and Newman, S. and Jones, T. and F. The. 2011 , month = jun, journal =. doi:10.1088/0004-637X/733/2/101 , keywords =

    work page doi:10.1088/0004-637x/733/2/101 2011

  57. [57]

    Goldreich, P. and. I. 1965 , month = jan, journal =. doi:10.1093/mnras/130.2.97 , annotation =

    work page doi:10.1093/mnras/130.2.97 1965

  58. [58]

    Goldreich, P. and. 1965 , month = jan, journal =. doi:10.1093/mnras/130.2.125 , annotation =

    work page doi:10.1093/mnras/130.2.125 1965

  59. [59]

    Multiwavelength

    Gong, Jun-Yu and Mao, Ye-Wei and Gao, Hua and Yu, Si-Yue , year =. Multiwavelength. The Astrophysical Journal Supplement Series , volume =. doi:10.3847/1538-4365/acd554 , keywords =

    work page doi:10.3847/1538-4365/acd554

  60. [60]

    and Cassata, Paolo and Koekemoer, Anton M

    Guo, Yicheng and Giavalisco, Mauro and Ferguson, Henry C. and Cassata, Paolo and Koekemoer, Anton M. , year =. Multi-Wavelength. The Astrophysical Journal , volume =. doi:10.1088/0004-637X/757/2/120 , keywords =

    work page doi:10.1088/0004-637x/757/2/120

  61. [61]

    and Bell, Eric F

    Guo, Yicheng and Ferguson, Henry C. and Bell, Eric F. and Koo, David C. and Conselice, Christopher J. and Giavalisco, Mauro and Kassin, Susan and Lu, Yu and Lucas, Ray and Mandelker, Nir and McIntosh, Daniel H. and Primack, Joel R. and Ravindranath, Swara and Barro, Guillermo and Ceverino, Daniel and Dekel, Avishai and Faber, Sandra M. and Fang, Jerome J....

    work page doi:10.1088/0004-637x/800/1/39

  62. [62]

    and Conselice, Christopher J

    Guo, Yicheng and Rafelski, Marc and Bell, Eric F. and Conselice, Christopher J. and Dekel, Avishai and Faber, S. M. and Giavalisco, Mauro and Koekemoer, Anton M. and Koo, David C. and Lu, Yu and Mandelker, Nir and Primack, Joel R. and Ceverino, Daniel and. Clumpy. 2018 , month = feb, journal =. doi:10.3847/1538-4357/aaa018 , keywords =

    work page doi:10.3847/1538-4357/aaa018 2018

  63. [63]

    and Bamford, Steven P

    Hart, Ross E. and Bamford, Steven P. and Hayes, Wayne B. and Cardamone, Carolin N. and Keel, William C. and Kruk, Sandor J. and Lintott, Chris J. and Masters, Karen L. and Simmons, Brooke D. and Smethurst, Rebecca J. , year =. Galaxy. Monthly Notices of the Royal Astronomical Society , volume =. doi:10.1093/mnras/stx2137 , keywords =

    work page doi:10.1093/mnras/stx2137

  64. [64]

    ACS Data Handbook v. 13.0. ACS Data Handbook v. 13.0 , year = 2024, volume =

    work page 2024

  65. [65]

    2013 , month = mar, journal =

    H. 2013 , month = mar, journal =. doi:10.1093/mnras/sts633 , keywords =

    work page doi:10.1093/mnras/sts633 2013

  66. [66]

    Hodge, J. A. and Swinbank, A. M. and Simpson, J. M. and Smail, I. and Walter, F. and Alexander, D. M. and Bertoldi, F. and Biggs, A. D. and Brandt, W. N. and Chapman, S. C. and Chen, C. C. and Coppin, K. E. K. and Cox, P. and Dannerbauer, H. and Edge, A. C. and Greve, T. R. and Ivison, R. J. and Karim, A. and Knudsen, K. K. and Menten, K. M. and Rix, H.-W...

    work page doi:10.3847/1538-4357/833/1/103 2016

  67. [67]

    Hodge, J. A. and. High-Redshift Star Formation in the. 2020 , month = dec, journal =. doi:10.1098/rsos.200556 , keywords =

    work page doi:10.1098/rsos.200556 2020

  68. [68]

    and Bundy, Kevin and Croton, Darren and Hernquist, Lars and Keres, Dusan and Khochfar, Sadegh and Stewart, Kyle and Wetzel, Andrew and Younger, Joshua D

    Hopkins, Philip F. and Bundy, Kevin and Croton, Darren and Hernquist, Lars and Keres, Dusan and Khochfar, Sadegh and Stewart, Kyle and Wetzel, Andrew and Younger, Joshua D. , year =. Mergers and. The Astrophysical Journal , volume =. doi:10.1088/0004-637X/715/1/202 , keywords =

    work page doi:10.1088/0004-637x/715/1/202

  69. [69]

    , archivePrefix = "arXiv", eprint =

    Stellar Feedback and Bulge Formation in Clumpy Discs , author =. 2012 , month = dec, journal =. doi:10.1111/j.1365-2966.2012.21981.x , keywords =

    work page doi:10.1111/j.1365-2966.2012.21981.x 2012

  70. [70]

    2015 , month = aug, journal =

    Revisiting the Original Morphology-Density Relation , author =. 2015 , month = aug, journal =. doi:10.1093/mnras/stv1113 , keywords =

    work page doi:10.1093/mnras/stv1113 2015

  71. [71]

    2020 , month = nov, journal =

    Stellar Masses of Giant Clumps in. 2020 , month = nov, journal =. doi:10.1093/mnras/staa2777 , keywords =

    work page doi:10.1093/mnras/staa2777 2020

  72. [72]

    and Zavala, Jorge A

    Ikeda, Ryota and Iono, Daisuke and Tadaki, Ken-ichi and Franco, Maximilien and Yun, Min S. and Zavala, Jorge A. and Tamura, Yoichi and Tsukui, Takafumi and Williams, Christina C. and Hatsukade, Bunyo and Lee, Minju M. and Michiyama, Tomonari and Mitsuhashi, Ikki and Nakanishi, Kouichiro and Casey, Caitlin M. and Ikarashi, Soh and Lee, Kianhong and Matsuda...

    work page doi:10.48550/arxiv.2510.18006

  73. [73]

    Non-Linear Violent Disc Instability with High

    Inoue, Shigeki and Dekel, Avishai and Mandelker, Nir and Ceverino, Daniel and Bournaud, Fr. Non-Linear Violent Disc Instability with High. Monthly Notices of the Royal Astronomical Society , volume =. doi:10.1093/mnras/stv2793 , keywords =

    work page doi:10.1093/mnras/stv2793

  74. [74]

    Spiral-Arm Instability: Giant Clump Formation via Fragmentation of a Galactic Spiral Arm , shorttitle =

    Inoue, Shigeki and Yoshida, Naoki , year =. Spiral-Arm Instability: Giant Clump Formation via Fragmentation of a Galactic Spiral Arm , shorttitle =. Monthly Notices of the Royal Astronomical Society , volume =. doi:10.1093/mnras/stx2978 , keywords =

    work page doi:10.1093/mnras/stx2978

  75. [75]

    1984 , month = jan, journal =

    Two-Fluid Gravitational Instabilities in a Galactic Disk , author =. 1984 , month = jan, journal =. doi:10.1086/161597 , keywords =

    work page doi:10.1086/161597 1984

  76. [76]

    and Leja, Joel and Conroy, Charlie and Speagle, Joshua S

    Johnson, Benjamin D. and Leja, Joel and Conroy, Charlie and Speagle, Joshua S. , year =. Stellar. The Astrophysical Journal Supplement Series , volume =. doi:10.3847/1538-4365/abef67 , keywords =

    work page internal anchor Pith review doi:10.3847/1538-4365/abef67

  77. [77]

    and Toomre, Alar , year =

    Julian, William H. and Toomre, Alar , year =. Non-. The Astrophysical Journal , volume =. doi:10.1086/148957 , annotation =

    work page doi:10.1086/148957

  78. [78]

    and Yamada, T

    Kajisawa, M. and Yamada, T. , year =. Evolution of the. The Astrophysical Journal , volume =. doi:10.1086/425957 , keywords =

    work page doi:10.1086/425957

  79. [79]

    and Silverman, John D

    Kalita, Boris S. and Silverman, John D. and Daddi, Emanuele and Bottrell, Connor and Ho, Luis C. and Ding, Xuheng and Yang, Lilan , year =. A. The Astrophysical Journal , volume =. doi:10.3847/1538-4357/acfee4 , keywords =

    work page doi:10.3847/1538-4357/acfee4

  80. [80]

    2025 , month = jan, journal =

    Clumps as Multiscale Structures in Cosmic Noon Galaxies , author =. 2025 , month = jan, journal =. doi:10.1093/mnras/stae2781 , keywords =

    work page doi:10.1093/mnras/stae2781 2025

Showing first 80 references.