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arxiv: 2606.13391 · v1 · pith:ERG5BY2Xnew · submitted 2026-06-11 · 🌌 astro-ph.GA

Feedback in Extragalactic Star Clusters (FEAST): Spectral Energy Distributions and the Physical Properties of Star Clusters in NGC 628 with CIGALE

Sean T. Linden , Angela Adamo , Alex Pedrini , Daniela Calzetti , Helena Faustino Vieira , Bruce E. Elmegreen , John S. Gallagher , Kelsey Johnson
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Matteo Messa Kathryn Grasha Ana Duarte-Cabral Arjan Bik Giacomo Bortolini Matteo Correnti Drew Lapeer Thomas S.-Y. Lai Goran Ostlin Linda J. Smith Monica Tosi
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Pith reviewed 2026-06-27 06:30 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords star clustersSED fittingNGC 628emerging young star clustersPAH emissionPDR clearingJWSTdust extinction
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The pith

Star clusters in NGC 628 clear surrounding dust in about 4 million years.

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

This paper fits spectral energy distributions to over 12,000 star clusters observed in NGC 628 with Hubble and James Webb telescopes. It identifies emerging young star clusters still partly hidden by dust and shows they reach peak numbers at ages of 3 to 5 million years. The fits reveal an evolutionary path from sources with compact PAH emission to those with diffuse emission as clusters clear their gas and dust, yielding a clearing timescale of roughly 4 million years. Clusters in spiral arms tend to be more massive and more reddened than those in inter-arm regions.

Core claim

SED fitting with CIGALE on HST and JWST data from 0.3 to 7.7 microns shows eYSC-I and eYSC-II populations peak at 3-5 Myr, with 12 percent having E(B-V) > 2. Distributions of q_PAH and the stellar-to-nebular attenuation ratio E(B-V)_star/E(B-V)_neb indicate an evolutionary sequence from eYSC-I to eYSC-II. The ratio of eYSC-I to optically visible clusters implies a PDR clearing timescale of ~4 Myr. Spiral-arm clusters are preferentially more massive and dust-reddened, and ~65 percent of eYSC-I align with F770W peaks.

What carries the argument

The number ratio of eYSC-I sources to optically visible stellar clusters, which directly yields the photo-dissociation region clearing timescale of ~4 Myr.

If this is right

  • Spiral-arm clusters form more massive and dust-reddened than inter-arm clusters.
  • ~65% of eYSC-I, ~27% of eYSC-II, and ~40% of F335M sources coincide with F770W peaks, confirming they trace the youngest regions.
  • The evolutionary sequence from eYSC-I to eYSC-II follows from shifts in PAH fraction and attenuation ratio as dust clears.
  • JWST data plus CIGALE grids can isolate the brief embedded phase of cluster emergence.

Where Pith is reading between the lines

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

  • The same ratio method could be applied to other galaxies to test whether the 4 Myr clearing time is universal.
  • The arm-interarm mass and reddening difference may reflect higher gas densities driving more embedded formation in arms.
  • Higher-resolution or spectroscopic follow-up could confirm whether the q_PAH and attenuation trends hold across the full cluster population.

Load-bearing premise

That the CIGALE SED model grids accurately represent the physical properties of young, dust-embedded star clusters without significant systematic biases in derived ages, extinctions, or evolutionary classifications.

What would settle it

Spectroscopic age measurements that fail to show eYSC-I and eYSC-II populations peaking at 3-5 Myr, or a number ratio of eYSC-I to visible clusters that deviates from the value expected for a 4 Myr clearing time under steady formation.

Figures

Figures reproduced from arXiv: 2606.13391 by Alex Pedrini, Ana Duarte-Cabral, Angela Adamo, Arjan Bik, Bruce E. Elmegreen, Daniela Calzetti, Drew Lapeer, Giacomo Bortolini, Goran Ostlin, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey Johnson, Linda J. Smith, Matteo Correnti, Matteo Messa, Monica Tosi, Sean T. Linden, Thomas S.-Y. Lai.

Figure 1
Figure 1. Figure 1: Examples of spectral energy distribution (SED) fits for representative eYSC-I (Left) and eYSC-II (Right) sources identified in NGC 628. The solid black line shows the best-fitting cigale model, with the unattenuated (attenuated) stellar emission shown in blue (yellow), nebular emission in green, and the dust emission in red. The observed and model fluxes corresponds to the purple and red points respectivel… view at source ↗
Figure 2
Figure 2. Figure 2: Left: The fractional residuals between our observed optically-selected star cluster catalog and the best-fitting model fluxes based on cigale when restricted to λ < 2 µm to better-match SSP models which do not include any contributions from hot dust or PAH emission. Middle: Histograms of the difference in the derived age of optically-selected star clusters in NGC 628 relative to Yggdrasil stellar populatio… view at source ↗
Figure 3
Figure 3. Figure 3: The near-IR color–color diagram of eYSC-I (red), eYSC-II (orange), and F335M-selected (green) sources in NGC 628 using F150W-F200W and F200W-F335M colors with the median value for each distribution shown as a square, pentagon, and triangle respectively. Overlaid in dark blue is a Yggdrasil SSP model track with solar metallicity and a Kroupa IMF (Kroupa 2001). In light blue we show the same SSP model track … view at source ↗
Figure 4
Figure 4. Figure 4: Results of the full cigale SED fitting for eYSC candidates in NGC 628. Panels show the distributions of best-fit ages (Left), stellar masses (Middle), and extinction E(B−V ) (Right). The distribution of ages for eYSC-I and II sources peaks at ∼ 3 − 5 Myr. eYSC sources in NGC 628 have masses from 103 –104 M⊙, with a wide range of extinctions peaking at ∼ 0.5 and extending to values as high as E(B−V ) = 3. D… view at source ↗
Figure 5
Figure 5. Figure 5: Comparison between the best-fit ages (Left), extinction E(B−V ) (Middle), and qPAH (Right) of our F770W￾selected sources (grey histogram) which overlap an eYSC-I, II, or F335M-selected source within 4 pixels. Using the same model grid adopted for our emerging cluster catalogs, the fits extend out to 7.7µm to include F560W and F770W observations with MIRI. In red, yellow, and green we show the individual di… view at source ↗
Figure 6
Figure 6. Figure 6: Distributions of dust and attenuation properties for emerging clusters in NGC 628 derived from cigale. Left: Fractional PAH abundance (qPAH) for clusters identified as eYSC-I (red), eYSC-II (orange), and F335M-selected (green) sources. The distribution of qPAH peaks at systematically lower values relative to eYSC-I sources. Right: Ratio of nebular to stellar continuum attenuation, E(B−V )⋆/E(B−V )neb, whic… view at source ↗
Figure 7
Figure 7. Figure 7: Near- and mid-IR color–color comparison of our F770W-selected sources which overlap eYSC-I, II and F335M￾selected sources within 4 NIRcam pixels (gray points). Magenta and turquoise squares are 3.3µm-bright sources identified Rodr´ıguez et al. (2025). The distribution of F770W-selected sources closely aligns with the compact 3.3 µm PAH emitters identified by Rodr´ıguez et al. (2025), confirming that F770W … view at source ↗
Figure 8
Figure 8. Figure 8: Comparison of the derived eYSC best-fit ages (Left), stellar masses (Middle), and extinction E(B−V ) (Right) for sources falling in arm (solid lines) and inter-arm (dashed-lines) regions using the environmental mask of Querejeta et al. (2021). Although the age distributions appear broadly consistent, star clusters that reside in the spiral arms of NGC 628 appear to be systematically more massive (∼0.1–0.2 … view at source ↗
Figure 9
Figure 9. Figure 9: ). However, we also find that the inferred stellar masses are systematically higher (∼ 0.4 dex) than seen in the middle Panel of [PITH_FULL_IMAGE:figures/full_fig_p019_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Residuals from SED fitting when including all HST and JWST NIRCam observations (Left), as well as JWST MIRI photometry (Right). The addition of mid-IR F560W and F770W observations help to reduce the overall scatter from 3–8 µm, and confirms that hot dust and PAH emission must be included to reproduce the youngest clusters [PITH_FULL_IMAGE:figures/full_fig_p020_10.png] view at source ↗
read the original abstract

With Hubble Space Telescope (HST) and James Webb Space Telescope (JWST) observations of NGC~628 spanning 0.3--7.7\,$\mu$m, we fit the spectral energy distributions (SEDs) of over 12,000 optically-selected star clusters, emerging young star clusters (eYSCs), and MIRI-selected sources with \textsc{cigale} to derive their ages, masses, extinctions, and dust properties. We find that near-infrared selected eYSC-I (compact Pa$\alpha$ and 3.3,$\mu$m PAH emission) and eYSC-II (compact Pa$\alpha$ and diffuse 3.3,$\mu$m PAH emssion) sources peak at $\sim$3--5~Myr, where $\sim 12\%$ of the clusters have an $E(B{-}V)>2$, demonstrating the presence of dust-embedded populations as clusters emerge. Further, the distributions of the fractional polycyclic aromatic hydrocarbon (PAH) abundance ($q_{\mathrm PAH}$) and stellar-to-nebular attenuation ratio ($E(B{-}V)_{{\rm \star}}/E(B{-}V)_{\rm neb}$) suggest an evolutionary sequence in which sources evolve from eYSC-I to eYSC-II as clusters clear their surrounding dust and gas. The photo-dissociation region (PDR) clearing timescale inferred from the ratio of eYSC-I to optically visible stellar clusters is $\sim$4~Myr. Additionally, we find that star clusters in the spiral arms of NGC 628 are preferentially more massive and more dust-reddened than those in inter-arm regions.~Finally, we find that $\sim$65\% of eYSC-I, $\sim$27\% of eYSC-II, and $\sim$40\% of F335M-selected sources coincide with an F770W peak in our MIRI-selected catalog within 4 pixels, confirming that F770W-bright sources preferentially trace the youngest and dustiest regions. Overall, our results highlight the ability of JWST together with \textsc{cigale} model grids to identify and characterize eYSCs during their short-lived embedded phases, and provide constraints on the feedback mechanisms that govern the emergence of stellar clusters.

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 / 2 minor

Summary. The manuscript fits SEDs of over 12,000 star clusters, eYSCs, and MIRI sources in NGC 628 using CIGALE on 0.3–7.7 μm HST/JWST photometry. It reports ages, masses, extinctions, and dust properties, with eYSC-I and eYSC-II populations peaking at ∼3–5 Myr and ∼12% of clusters having E(B−V)>2. The paper infers a ∼4 Myr PDR clearing timescale from the eYSC-I to optically visible cluster ratio, proposes an evolutionary sequence from the q_PAH and E(B−V)_star/E(B−V)_neb distributions, notes arm/inter-arm differences, and reports spatial coincidences with F770W peaks.

Significance. If the CIGALE-derived parameters and classifications are robust, the large sample and JWST-enabled identification of embedded phases provide useful empirical constraints on cluster feedback and emergence timescales. The multi-wavelength coverage and focus on the short-lived embedded stage are strengths.

major comments (2)
  1. [Abstract] Abstract: the PDR clearing timescale of ∼4 Myr is inferred directly from the observed ratio of eYSC-I to optically visible clusters; this ratio is load-bearing on the CIGALE age and classification assignments, yet the manuscript supplies no validation (e.g., recovery tests on mock SEDs with clumpy dust or bursty SFH) that the standard modules do not systematically bias ages or extinctions for compact, embedded sources.
  2. [Abstract] Abstract: the claimed evolutionary sequence from the q_PAH and E(B−V)_star/E(B−V)_neb distributions likewise rests on the fidelity of the fitted parameters; without explicit checks that the model grids (continuous/exponentially declining SFH, screen/mixed geometries) accurately recover input values for dust-embedded clusters, the sequence could be an artifact of fitting biases.
minor comments (2)
  1. [Abstract] Abstract: 'emssion' is a typo and should read 'emission'.
  2. [Abstract] Abstract: '3.3,$μm$' uses an incorrect comma separator; standard notation is 3.3 μm.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thoughtful review and for highlighting the importance of validating the CIGALE-derived parameters. We respond to each major comment below, providing clarification on how the classifications and inferences are supported by the data while acknowledging areas where additional discussion can be added.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the PDR clearing timescale of ∼4 Myr is inferred directly from the observed ratio of eYSC-I to optically visible clusters; this ratio is load-bearing on the CIGALE age and classification assignments, yet the manuscript supplies no validation (e.g., recovery tests on mock SEDs with clumpy dust or bursty SFH) that the standard modules do not systematically bias ages or extinctions for compact, embedded sources.

    Authors: The eYSC-I population is defined observationally by the presence of compact Paα and 3.3 μm PAH emission, independent of the CIGALE age or extinction outputs. The PDR clearing timescale is derived from the ratio of the number of these observationally selected eYSC-I sources to the number of optically visible clusters; the CIGALE ages are reported separately and show a peak at 3–5 Myr that is consistent with the selection but not required for the ratio itself. We agree that explicit mock recovery tests for clumpy dust geometries would strengthen confidence in the fitted parameters for the most embedded sources. In the revised manuscript we will add a dedicated paragraph discussing the applicability of the standard CIGALE modules to embedded clusters and citing existing validation studies in the literature. revision: partial

  2. Referee: [Abstract] Abstract: the claimed evolutionary sequence from the q_PAH and E(B−V)_star/E(B−V)_neb distributions likewise rests on the fidelity of the fitted parameters; without explicit checks that the model grids (continuous/exponentially declining SFH, screen/mixed geometries) accurately recover input values for dust-embedded clusters, the sequence could be an artifact of fitting biases.

    Authors: The q_PAH and stellar-to-nebular attenuation ratio distributions are indeed outputs of the CIGALE fits. However, the proposed evolutionary sequence is also corroborated by the independent observational distinction between eYSC-I (compact PAH) and eYSC-II (diffuse PAH) sources. We acknowledge that the current manuscript does not present dedicated recovery tests using mock SEDs with the exact model grid choices for highly embedded objects. We will therefore expand the methods and discussion sections to include a brief assessment of possible fitting biases for dust-embedded clusters and to note how the multi-wavelength constraints (including the Paα and PAH imaging) help mitigate such biases. revision: yes

Circularity Check

0 steps flagged

No circularity: standard SED fitting to independent multi-band observations yields derived properties and ratios

full rationale

The derivation chain begins with direct observational classifications (eYSC-I/II defined by compact Paα + 3.3 μm PAH features) and number counts from HST/JWST imaging, followed by CIGALE fits to the same independent photometry to extract ages, E(B-V), q_PAH, and attenuation ratios. The ~4 Myr PDR timescale is computed from the observed eYSC-I to optically visible cluster ratio; the evolutionary sequence is read from the empirical distributions of fitted q_PAH and E(B-V)_star/E(B-V)_neb. None of these steps reduce a claimed prediction to a fitted input by construction, invoke self-citation for a uniqueness theorem, or smuggle an ansatz. The analysis is self-contained against external data and standard model grids.

Axiom & Free-Parameter Ledger

4 free parameters · 2 axioms · 0 invented entities

The central claims rest on the accuracy of CIGALE stellar population and dust models for interpreting multi-wavelength photometry of young clusters. Numerous parameters in these models are adjusted during fitting. No new physical entities are introduced.

free parameters (4)
  • cluster age
    Fitted parameter in SED models to match observed fluxes.
  • stellar mass
    Derived by scaling model luminosity to observed fluxes.
  • E(B-V) extinction
    Fitted separately for stellar and nebular components.
  • q_PAH
    Fractional PAH abundance fitted in dust emission models.
axioms (2)
  • domain assumption CIGALE model grids provide unbiased representations of the SEDs of star clusters aged 1-10 Myr with varying dust content.
    Fitting procedure assumes these models capture the relevant physics for deriving ages and extinctions.
  • domain assumption Source selection criteria reliably identify star clusters in NGC 628 rather than contaminants or background objects.
    Optical and MIRI selections are taken as corresponding to the intended populations.

pith-pipeline@v0.9.1-grok · 6056 in / 1594 out tokens · 39495 ms · 2026-06-27T06:30:14.966675+00:00 · methodology

discussion (0)

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