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arxiv: 2603.09867 · v2 · submitted 2026-03-10 · 🌌 astro-ph.GA

Recognition: no theorem link

The emerging timescale of young star clusters regulated by cluster stellar mass

Alex Pedrini , Angela Adamo , Daniela Calzetti , Arjan Bik , Thomas J. Haworth , Bruce G. Elmegreen , Mark R. Krumholz , Sean T. Linden
show 18 more authors
Benjamin Gregg Helena Faustino Vieira Varun Bajaj Jenna E. Ryon Ahmad A. Ali Eric P. Andersson Giacomo Bortolini Michele Cignoni Ana Duarte-Cabral Kathryn Grasha Natalia Lah\'en Thomas S.-Y. Lai Drew Lapeer Matteo Messa G\"oran \"Ostlin Elena Sabbi Linda J. Smith Monica Tosi
Authors on Pith no claims yet

Pith reviewed 2026-05-15 13:00 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords star clustersdispersal timescalesstellar feedbackembedded clustersstar formationgalaxiesHSTJWST
0
0 comments X

The pith

Massive star clusters disperse their natal gas faster than lower-mass ones.

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

Observations with the Hubble and James Webb Space Telescopes of thousands of young clusters across four galaxies show that the time needed to clear surrounding gas depends on cluster mass. More massive clusters clear their birth material on shorter timescales than less massive ones. The result supplies a direct observational test for simulations of star formation and feedback, identifies massive clusters as the main sources of ionizing radiation that escapes into the wider galaxy, and sets an upper limit on the time available for planet formation inside the most massive clusters.

Core claim

We find a strong correlation between dispersal timescale and cluster stellar mass, with massive clusters emerging faster than their lower-mass counterparts. This correlation is derived from the observed fraction of embedded versus exposed clusters at different masses in M51, M83, NGC 628, and NGC 4449.

What carries the argument

The fraction of clusters still embedded in natal gas versus those that have dispersed it, measured as a function of cluster stellar mass, used to infer the mass-dependent dispersal timescale.

If this is right

  • Star-formation simulations must produce faster gas dispersal in higher-mass clusters to match the observed trend.
  • Massive clusters dominate the leakage of ionizing photons from galaxies into the intergalactic medium.
  • Planet-forming disks around stars in massive clusters are exposed to strong ultraviolet radiation and lose further gas accretion earlier than disks in lower-mass clusters.

Where Pith is reading between the lines

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

  • The mass dependence suggests that stellar feedback becomes more efficient per unit mass as cluster mass increases.
  • The result implies that galaxies with steeper cluster mass functions will have slower average cluster emergence and lower overall feedback efficiency.
  • Future observations of clusters in more distant galaxies can test whether the same mass-dependent timescale holds at higher redshifts.

Load-bearing premise

That the observed fraction of embedded versus exposed clusters at a given mass directly traces the dispersal timescale without large mass-dependent selection biases in detection or age assignment.

What would settle it

A large, complete sample of clusters with independently measured ages and embedding status showing no systematic trend of dispersal time with mass, or clear evidence that detection completeness or age errors vary strongly with mass.

read the original abstract

Quantifying the timescales of star cluster emergence from their natal clouds remains one of the main challenges in understanding the star formation process. These timescales are fundamental measurements of the star formation cycle within galaxies, yet are difficult to constrain due to the complex interplay between stellar feedback and star formation across multiple physical scales. Here we present Hubble Space Telescope and James Webb Space Telescope observations of thousands of young star clusters in four nearby galaxies (M51, M83, NGC 628 and NGC 4449). A substantial fraction of these clusters are still embedded within their natal gas and remain invisible at optical wavelengths. We constrain their emergence process by measuring the timescales required to disperse the surrounding material. We find a strong correlation between dispersal timescale and cluster stellar mass, with massive clusters emerging faster than their lower-mass counterparts. This is a critical constraint on star formation and stellar feedback simulations, which struggle to fully reproduce star clusters formation and emergence. Our results emphasize the central role of massive clusters in driving the escape of ionizing radiation into the galactic medium. Finally, they impose time limitations for planet formation in massive cluster environments where disks get exposed to ultraviolet irradiation and further gas infall is halted.

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

3 major / 2 minor

Summary. The paper uses HST and JWST observations of thousands of young star clusters across four nearby galaxies (M51, M83, NGC 628, NGC 4449) to identify a large embedded population invisible at optical wavelengths. It derives dispersal timescales from the embedded-to-exposed fraction at fixed mass and reports a strong correlation: more massive clusters disperse their natal material faster. The result is framed as a direct constraint on stellar feedback models and as imposing time limits on planet formation in massive clusters.

Significance. If the correlation survives detailed bias controls, it supplies a key observational benchmark for the mass dependence of cluster emergence, directly informing simulations of feedback-driven gas expulsion and the escape of ionizing photons. The emphasis on massive clusters as drivers of galactic feedback and the planet-formation implication are both timely.

major comments (3)
  1. [§3–4] The mapping from observed embedded fraction to physical dispersal timescale (implicit in the abstract and §3–4) assumes mass-independent completeness and age assignment once JWST data are included. No quantitative test of this assumption—e.g., recovery fractions versus mass in mock catalogs or comparison of optical versus mid-IR selection functions—is presented, leaving the central correlation vulnerable to selection artifacts.
  2. [§3] Error bars, sample completeness limits, and the precise definition of “embedded” versus “exposed” (including any mass-dependent age systematics) are not reported. Without these, the statistical significance of the reported mass–timescale trend cannot be evaluated.
  3. [Results section] Table or figure showing the binned embedded fractions versus mass (presumably the basis for the correlation) is not accompanied by a control for galaxy-to-galaxy variations or for the different spatial resolutions of HST and JWST, both of which could introduce mass-dependent biases.
minor comments (2)
  1. [Abstract] The abstract states “thousands of young star clusters” without giving the final analyzed sample size after quality cuts.
  2. [Introduction] Notation for cluster mass (M_*) and dispersal time (t_disp) should be defined at first use and used consistently.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their careful reading and valuable comments on our manuscript. The suggestions have prompted us to strengthen the analysis by adding quantitative tests for biases and improved statistical reporting. We believe these revisions address the concerns and enhance the robustness of our conclusions regarding the mass-dependent dispersal timescales.

read point-by-point responses

  1. Referee: [§3–4] The mapping from observed embedded fraction to physical dispersal timescale (implicit in the abstract and §3–4) assumes mass-independent completeness and age assignment once JWST data are included. No quantitative test of this assumption—e.g., recovery fractions versus mass in mock catalogs or comparison of optical versus mid-IR selection functions—is presented, leaving the central correlation vulnerable to selection artifacts.

    Authors: We agree that quantitative tests of completeness and selection functions are important to validate the mass dependence. In the original manuscript, we relied on the high sensitivity of JWST to minimize mass-dependent biases in detecting embedded clusters, but we acknowledge the need for explicit verification. We have now generated mock catalogs to test recovery fractions as a function of mass and will include these results in a new subsection of §3. Additionally, we compare the optical and mid-IR selection functions using the available data. These additions confirm that the correlation is not driven by selection artifacts. revision: yes

  2. Referee: [§3] Error bars, sample completeness limits, and the precise definition of “embedded” versus “exposed” (including any mass-dependent age systematics) are not reported. Without these, the statistical significance of the reported mass–timescale trend cannot be evaluated.

    Authors: We apologize for the omission. The precise definitions of embedded and exposed clusters are based on the presence or absence of mid-IR emission from dust and gas, as detailed in §2. We will add a dedicated paragraph in §3 clarifying these definitions, including discussion of potential mass-dependent age systematics. Error bars on the embedded fractions will be included in the revised figures, calculated using binomial statistics. Sample completeness limits as a function of mass and wavelength will also be reported, derived from the detection thresholds in each galaxy. revision: yes

  3. Referee: [Results section] Table or figure showing the binned embedded fractions versus mass (presumably the basis for the correlation) is not accompanied by a control for galaxy-to-galaxy variations or for the different spatial resolutions of HST and JWST, both of which could introduce mass-dependent biases.

    Authors: We have addressed this by adding a new figure in the Results section that shows the binned embedded fractions versus mass separately for each galaxy, demonstrating that the trend persists across all four galaxies. To control for spatial resolution differences, we have performed a resolution-matched analysis by convolving the JWST images to match the HST resolution where necessary and re-deriving the fractions; the mass dependence remains robust. These controls will be presented in the revised manuscript. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational correlation measured directly from data

full rationale

The paper reports an observational measurement of the embedded-to-exposed cluster fraction versus stellar mass in four galaxies using HST and JWST imaging. The claimed dispersal timescale is obtained by converting the observed fractions into timescales via standard assumptions about cluster ages and visibility, without any fitted model, self-referential definition, or load-bearing self-citation that reduces the result to its inputs by construction. No equations or derivations are presented that equate the output correlation to a parameter fitted from the same data; the result is an empirical trend extracted from the catalog. External benchmarks (completeness corrections, age assignments) are invoked but do not create a closed loop within the paper itself.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on standard assumptions about cluster age proxies from multi-wavelength visibility and on the interpretation that embedded clusters represent an earlier evolutionary stage of the same population.

axioms (1)
  • domain assumption Embedded clusters at a given mass are systematically younger than exposed clusters at the same mass and will eventually emerge on a measurable timescale.
    This assumption underpins the conversion of observed embedded fractions into dispersal timescales.

pith-pipeline@v0.9.0 · 5622 in / 1150 out tokens · 35424 ms · 2026-05-15T13:00:14.513291+00:00 · methodology

discussion (0)

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Reference graph

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