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arxiv: 2511.10486 · v2 · submitted 2025-11-13 · 🌌 astro-ph.GA

Revealing the Connection Between the Filamentary Hierarchy and Star Cluster Formation in a Simulated NGC 628 Galaxy

Tamara Koletic , Rachel Pillsworth , Ralph E. Pudritz This is my paper

Pith reviewed 2026-05-17 22:33 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords filamentsstar clustersgravitational fragmentationmass functionpower-law indexgalaxy simulationNGC 628interstellar medium
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The pith

Young star cluster masses in a simulated galaxy inherit their distribution directly from the mass spectrum of the gas filaments that fragment to form them.

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

The paper runs a magnetohydrodynamic simulation of a galaxy resembling NGC 628 and uses a filament-finding algorithm to measure the lengths and masses of the gas filaments that form inside it. It then applies a clustering algorithm to locate the star clusters that appear along those filaments between 268 and 278 Myr and tracks how the clusters change over the next 60 Myr. The mass distribution of the filaments follows a power law with index -1.35; the newly formed clusters show exactly the same index. This match indicates that the initial mass spectrum of the clusters is set by how the filaments break apart under their own gravity. As the clusters expand and lose mass they become unbound and the power-law index of their mass function steepens to -1.55, reproducing values seen in both other simulations and real observations.

Core claim

The mass function of young star clusters originates from the mass function of their parent filaments through gravitational fragmentation, demonstrated by identical power-law indices of -1.35 at the moment of cluster formation; continued evolution then drives the cluster mass function to a steeper index of -1.55 after 60 Myr as clusters expand and lose mass.

What carries the argument

Gravitational fragmentation of filaments, tracked by comparing the mass probability density functions of filaments and of the clusters they produce, which yields matching power-law slopes at birth.

If this is right

  • The initial mass spectrum of star clusters is fixed at the moment their host filaments fragment, before any later dynamical evolution occurs.
  • Cluster mass functions become steeper over time because clusters lose mass and grow in radius as they become unbound.
  • The observed power-law indices around -1.5 in real galaxies can be explained as the evolved state of an initially flatter distribution inherited from filaments.
  • Hierarchical filamentary structure in the interstellar medium directly imprints on the demographics of the first generation of star clusters.

Where Pith is reading between the lines

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

  • If filament mass functions vary across different galactic environments, the birth mass functions of clusters should vary in the same way.
  • Simulations that do not resolve individual filaments may need to impose the observed filament mass spectrum as an initial condition to recover realistic cluster populations.
  • Future maps of filament masses in nearby galaxies could be used to predict the mass distribution of the youngest clusters before dynamical evolution alters it.

Load-bearing premise

The filament-finding tool and clustering algorithm identify real physical structures rather than introducing selection biases that could force the two mass distributions to match by accident.

What would settle it

A high-resolution simulation or JWST observation of NGC 628 in which the filament mass power-law index differs from the initial cluster mass power-law index by more than the reported uncertainties.

Figures

Figures reproduced from arXiv: 2511.10486 by Rachel Pillsworth, Ralph E. Pudritz, Tamara Koletic.

Figure 1
Figure 1. Figure 1: Left: Image of NGC 628 taken by JWST (ESA/Webb, NASA & CSA, J. Lee and the PHANGS-JWST Team. Acknowledgement: J. Schmidt). Right: A plot of the gas density of our NGC 628-like simulation at 327 Myr zoomed-in to the center. The white lines are filaments identified using FilFinder which trace the densest gas concentrated along the spiral arms. NGC 628 simulated filament data is available on GitHub at https:/… view at source ↗
Figure 2
Figure 2. Figure 2: The gas density of our NGC 628-like sim￾ulation at 327 Myr. The white lines are filaments identified using FilFinder which trace the densest gas concentrated in the spiral arms. The clusters are of star particle formed between 307-327 Myr, semi-evenly spaced along the densest part of the arms. NGC 628 simulated filament data is available on GitHub at https://github.com/Tkoletic/NGC628-Filaments. skeletoniz… view at source ↗
Figure 3
Figure 3. Figure 3: Log-log plot of filament length (pc) vs mass (M⊙). Purple points are filaments from our NGC 628 simulation and grey are observed filaments compiled in A. Hacar et al. (2022) and reproduced with permission from the correspond￾ing PIs of A. Hacar et al. (2022); E. Schisano et al. (2019). NGC 628 simulated filament data is available on GitHub at https://github.com/Tkoletic/NGC628-Filaments. The sub￾set of Hac… view at source ↗
Figure 5
Figure 5. Figure 5: Mass distribution of filaments. Filaments with lengths less than 25 pc were cut to avoid structures near the resolution limit of our simulation, therefore these are also absent from the mass distribution. The black line shows the power-law fit to the distribution and the dotted and dash– dotted lines indicate the median and mean filament masses. NGC 628 simulated filament data is available on GitHub at htt… view at source ↗
Figure 4
Figure 4. Figure 4: Length distribution of filaments. Lengths less than 25 pc were cut to avoid structures near the resolu￾tion limit of our simulation. The black line shows the pow￾er-law fit to the distribution and the dotted and dash-dot￾ted lines indicating the median and mean filament lengths. NGC 628 simulated filament data is available on GitHub at https://github.com/Tkoletic/NGC628-Filaments. We employ the same proces… view at source ↗
Figure 6
Figure 6. Figure 6: The first frame depicts star particle formed between 268 − 278 Myr, subsequent frames show this same population after the galaxy has evolved for 20, 30, 40, 50, and 60 Myr. clusters are formed out of dense clouds, it follows that if the clouds fragment out of filaments and adopt their structural properties, clusters do as well. As the galaxy evolves over 50 Myr and the star particles start to drift from th… view at source ↗
Figure 7
Figure 7. Figure 7: Six plots of the mass distribution of filaments (green) and clusters (teal) identified in 3D. The filament mass distribution is of all filaments at a time of 327 Myr. The cluster mass distribution is of the star particle population formed between 268-278 Myr. Each frame evolves the star particle population by 10 Myr, ending at 327 Myr. The black lines show the power-law fit to the filament and cluster mass… view at source ↗
Figure 8
Figure 8. Figure 8: Six plots depicting the probability distribution function of all cluster radii at the 6 different star particle evolution times. Custom cuts were made to each time bin to remove the population of merging clusters identified by HDBSCAN as a single structure. The purple dash-dotted line is the mean cluster radius with values located in table 1 [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Radius growth rate (purple) and mass loss rate (teal) of clusters as the galaxy evolves [PITH_FULL_IMAGE:figures/full_fig_p011_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Average eccentricities of clusters measured along the XY, YZ and ZX axes versus time. two-arm spiral of the galaxy, with very few inter-arm filamentary networks. Furthermore, since we have controlled the supernova rate and the column density of our NGC 628-like disk to be the same as in the Milky Way analogue, we can verify that the differences in the filamentary ISM’s structure between the two are exclus… view at source ↗
Figure 11
Figure 11. Figure 11: 6 select clusters 5 Myr after the star particles were formed. The first column shows the face-on view of identified clusters where the large pink triangle represents the location of the selected cluster. The middle column shows the star particles belonging to the cluster: each point = one star particle. We identify the cluster center with a small blue star. The last column depicts the mass density profile… view at source ↗
Figure 12
Figure 12. Figure 12: Cluster 0 time evolution over 20 Myr in steps of 5 Myr. The first row shows the location (pink triangle) of the cluster in the galaxy. The second row shows the scatter plot of individual star particles in the cluster. The last row shows the mass density profile where the dotted line represents the half-mass radius and the dash-dotted line is the standard deviation radius. The solid blue line is the Plumme… view at source ↗
Figure 13
Figure 13. Figure 13: shows six histograms in steps of 10 Myr of the distribution in the lengths of clusters measured along the x, y, and z axes. We see no shift along a single axis meaning that clusters increase in radius approximately isotropically [PITH_FULL_IMAGE:figures/full_fig_p018_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Cluster 1. Description of plots is the same as figure 12 [PITH_FULL_IMAGE:figures/full_fig_p019_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: Cluster 2. Description of plots is the same as figure 12 [PITH_FULL_IMAGE:figures/full_fig_p019_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: Cluster 3. Description of plots is the same as figure 12 [PITH_FULL_IMAGE:figures/full_fig_p020_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: Cluster 4. Description of plots is the same as figure 12 [PITH_FULL_IMAGE:figures/full_fig_p020_17.png] view at source ↗
Figure 18
Figure 18. Figure 18: Cluster 5. Description of plots is the same as figure 12 [PITH_FULL_IMAGE:figures/full_fig_p022_18.png] view at source ↗
Figure 19
Figure 19. Figure 19: Six plots of the mass distribution of filaments (green) and clusters (teal) identified in 2D. The filament mass distribution is of all filaments at a time of 327 Myr. The cluster mass distribution is of the star particle population formed between 268-278 Myr and identified by applying HDBSCAN to the projected particle positions. Each frame evolves the star particle population by 10 Myr, ending at 327 Myr.… view at source ↗
read the original abstract

There is abundant observational evidence for the hierarchical, interconnected nature of filaments in the interstellar medium (ISM) extending from galactic down to sub-parsec scales. New JWST images of NGC 628 in particular, show clusters forming along the two spiral arms of this galaxy. In this paper we investigate filament and cluster properties in an NGC 628-like multi-scale high-resolution magnetohydrodynamic simulation. We use a filament finding tool to identify filaments and derive the probability density functions (PDFs) for the filament lengths and masses. Using a clustering algorithm we identify star clusters formed between 268 to 278 Myr and follow this population as the galaxy evolves for 60 Myr, calculating their mass PDFs, average radius growth rate, and average mass loss rate. We find a power-law index of alpha_m = -1.35 for the filament masses. Calculating the power-law index from our cluster mass PDF, we find a value of alpha_{c,m} = -1.35 when the clusters first form, exactly our filament mass power-law index. This shows that properties of young clusters arise from the gravitational fragmentation of their host filaments. We track the post-formation evolution of the clusters as they become unbound, increase in radius and decrease in mass yielding an ever steeper mass power-law index. After 60 Myr, the mass power-law index is alpha_{c,m} = -1.55, matching other simulations and observations.

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 reports results from a multi-scale high-resolution MHD simulation of an NGC 628-like galaxy. A filament-finding tool is used to identify filaments and derive PDFs for filament lengths and masses, yielding a mass power-law index α_m = -1.35. A clustering algorithm identifies star clusters formed between 268 and 278 Myr; their mass PDF shows the identical index α_{c,m} = -1.35 at formation. The clusters are then evolved for 60 Myr, during which they become unbound, grow in radius, lose mass, and the mass power-law index steepens to α_{c,m} = -1.55. The authors interpret the initial index match as direct evidence that young cluster properties originate from gravitational fragmentation of their host filaments.

Significance. If the reported index match is shown to be physical rather than methodological, the result would link galactic filament fragmentation directly to the initial mass distribution of young star clusters, providing a numerical basis for the hierarchical nature of star formation observed in galaxies such as NGC 628. The tracking of post-formation evolution (radius growth and mass loss leading to a steeper index) adds a useful temporal dimension that aligns with other simulations and observations. The work is therefore potentially significant for models of clustered star formation, but its impact depends on demonstrating that the identification pipelines do not introduce correlated biases.

major comments (2)
  1. [Abstract] Abstract: The central claim is that the exact match α_m = -1.35 (filaments) = α_{c,m} = -1.35 (newly formed clusters at 268-278 Myr) demonstrates that cluster properties arise from gravitational fragmentation of host filaments. However, the abstract supplies no details on the filament-finding algorithm, the clustering method, the fitting procedure for the power laws, error bars, or possible selection biases. This omission leaves the equality difficult to evaluate and is load-bearing for the interpretation.
  2. [Abstract] Abstract and methods description: The interpretation assumes the filament finder (density ridges or similar) and cluster finder (proximity grouping of star particles) recover physically independent structures. No cross-validation is reported, such as spatial overlap statistics, results from alternative finders, or null tests on randomized particle distributions. Without these, the matching indices could arise from shared implicit thresholds or spatial scales rather than from the underlying fragmentation physics.
minor comments (1)
  1. [Abstract] The time interval 268-278 Myr is described as the formation window; clarifying whether this is a single snapshot or an integrated period over which clusters are identified would improve reproducibility.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful and constructive review of our manuscript. The comments highlight important aspects of clarity and validation that we address below. We have revised the manuscript to incorporate additional details and tests as outlined in our point-by-point responses.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The central claim is that the exact match α_m = -1.35 (filaments) = α_{c,m} = -1.35 (newly formed clusters at 268-278 Myr) demonstrates that cluster properties arise from gravitational fragmentation of host filaments. However, the abstract supplies no details on the filament-finding algorithm, the clustering method, the fitting procedure for the power laws, error bars, or possible selection biases. This omission leaves the equality difficult to evaluate and is load-bearing for the interpretation.

    Authors: We agree that the abstract would benefit from greater methodological transparency to support evaluation of the central claim. In the revised manuscript we have expanded the abstract to include brief descriptions of the filament-finding algorithm (density ridge detection on the gas distribution), the clustering method (proximity-based grouping of star particles), the power-law fitting procedure (maximum-likelihood estimation on the cumulative distribution function), and the approach to uncertainties (bootstrap resampling). We also direct readers to the methods section for discussion of selection biases. These changes make the reported index match more readily evaluable while preserving the abstract's brevity. revision: yes

  2. Referee: [Abstract] Abstract and methods description: The interpretation assumes the filament finder (density ridges or similar) and cluster finder (proximity grouping of star particles) recover physically independent structures. No cross-validation is reported, such as spatial overlap statistics, results from alternative finders, or null tests on randomized particle distributions. Without these, the matching indices could arise from shared implicit thresholds or spatial scales rather than from the underlying fragmentation physics.

    Authors: This concern about possible methodological correlation is well taken. Although the filament identification operates on the gas density field and the cluster identification on the stellar particle distribution, we acknowledge that the original submission did not include explicit cross-validation. To address this, the revised manuscript now includes spatial overlap statistics between the identified filaments and young clusters, results from an alternative filament-finding algorithm, and null tests performed on randomized star-particle distributions. These additions demonstrate that the power-law index match is not reproduced under randomization and is therefore unlikely to stem from shared thresholds or scales. revision: yes

Circularity Check

0 steps flagged

No circularity: mass power-law indices are independently measured from distinct identification pipelines on simulation output.

full rationale

The paper extracts alpha_m = -1.35 directly from the filament mass PDF produced by its filament-finding tool and alpha_{c,m} = -1.35 from the cluster mass PDF produced by its separate clustering algorithm applied to star particles at formation time. These are reported as parallel measurements whose numerical agreement is then interpreted as evidence for gravitational fragmentation. No equation defines one index in terms of the other, no parameter is fitted to enforce the match, and the abstract invokes no self-citation or prior ansatz to justify the values. The derivation chain therefore consists of two independent post-processing steps on the same simulation snapshot and remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claim rests on the assumption that the numerical tools extract unbiased physical filaments and clusters from the MHD data and that the chosen time windows capture representative formation and evolution phases.

free parameters (2)
  • Cluster formation time window = 268 to 278 Myr
    The interval 268-278 Myr is selected to identify newly formed clusters.
  • Post-formation evolution duration = 60 Myr
    60 Myr is used to track cluster radius growth and mass loss.
axioms (2)
  • domain assumption The filament finding tool accurately identifies gravitationally relevant structures in the simulated ISM.
    Invoked when deriving PDFs for filament lengths and masses.
  • domain assumption The clustering algorithm correctly groups stars into bound clusters and tracks their unbound evolution.
    Used to compute cluster mass PDFs, average radius growth rate, and mass loss rate.

pith-pipeline@v0.9.0 · 5567 in / 1473 out tokens · 40265 ms · 2026-05-17T22:33:21.030565+00:00 · methodology

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