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The near infrared SED of young star clusters in the FEAST galaxies: Missing ingredients at 1-5 $\mu$m

T0 review · 3 major / 5 minor · reviewed 2026-08-05 · deepseek-v4-flash

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Pith's one-line read A systematic flux excess at 1.5–2.5 microns, strongest in young (≤6 Myr) low-mass (≤3000 solar masses) clusters, is not captured by current stellar population models; stochastic IMF sampling plus pre-main-sequence stars shrinks but does not

desk verdict Solid multi-galaxy measurement of a real NIR excess in young embedded clusters; the 'missing ingredients' interpretation is plausible but the nebular grid coverage caveat is not fully closed. read the letter →

arxiv 2509.01670 v1 pith:5O3FOLJI submitted 2025-09-01 astro-ph.GA

Alex Pedrini , Angela Adamo , Arjan Bik , Daniela Calzetti , Sean T. Linden , Benjamin Gregg , Varun Bajaj , Jenna E. Ryon
show 18 more authors
Anne S. M. Buckner Giacomo Bortolini Michele Cignoni Matteo Correnti Ana Duarte-Cabral Bruce G. Elmegreen Helena Faustino Vieira John S. Gallagher Kathryn Grasha Kelsey E. Johnson Mark R. Krumholz Drew Lapeer Thomas S. -Y. Lai Matteo Messa Göran Östlin Linn Roos Linda J. Smith Monica Tosi
This is my paper
classification astro-ph.GA
keywords StarclustersSpectralenergydistributionNear-infraredexcessEmbeddedyoungPre-main-sequencestarsStochasticIMFsamplingPolycyclicaromatichydrocarbonsJWSTNIRCam
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper uses combined HST and JWST photometry from 0.2 to 5 microns to fit the spectral energy distributions of about 3,800 emerging young star clusters in four nearby galaxies and claims that current stellar population models systematically underestimate their 1.5–2.5 micron flux. The excess is largest in the youngest (≤6 Myr) and least massive (≤3,000 solar masses) clusters, appears in the F150W and F200W (and F277W) bands, and survives tests with different apertures, different dust grids, and fits with dust emission removed. Stochastic sampling of the initial mass function with pre-main-sequence stars in the slug code moves model colors toward the observed ones but cannot close the gap in the metal-rich spirals. If the claim holds, SED-fit ages and masses of embedded young clusters are biased, and a fraction of strong Pa-alpha emitters are misclassified as older than 6 Myr. The paper concludes that emission from young stellar objects and more realistic IMF sampling are the missing ingredients.

What carries the argument

The load-bearing quantity is the per-filter residual Δm = m_model − m_observed, computed for thousands of eYSCs and summarized as medians in age/mass bins; positive Δm in F150W/F200W defines the NIR excess. The argument is carried by two SED tools: CIGALE, a deterministic fitting code using instantaneous-burst stellar populations, CLOUDY nebular emission, an attenuation law, and dust templates, and slug, a stochastic stellar-population synthesis code that samples the IMF and includes pre-main-sequence stars. The paired Pa-alpha equivalent-width age comparison provides an independent clock that exposes the age bias.

What would settle it

Take spectra of about ten low-mass (≤3,000 solar masses) clusters with SED-fitted ages ≤3 Myr in M51 over 1.4–2.6 µm with JWST/NIRSpec. If the observed continuum matches a stellar-plus-nebular model within a few percent band by band, the excess is a photometric or modeling artifact; if a broad smooth excess remains above the model and is not Pa-alpha, the missing component is physical.

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Extended reading notes

Core claim

The central discovery is a systematic near-infrared excess: observed fluxes in the 1.5 and 2.0 micron JWST bands exceed the best-fit model fluxes by roughly 0.2–0.6 mag for the young, low-mass subpopulation, while neighboring blue and red bands are fit well. The excess is strongest for clusters fitted with ages ≤3 Myr and masses ≤3,000 solar masses, and in every galaxy it persists when dust emission is removed from the fit and when smaller apertures are used. As a consequence, the fitting code assigns ages ≥6 Myr to a subset of clusters whose Pa-alpha equivalent widths indicate much younger ages, and it prefers dust parameters that are not those expected from mid/far-infrared studies of star

Load-bearing premise

The load-bearing premise is that the grid of ionized-gas models used in the fitting covers all realistically strong nebular continuum at 1.5–2.5 microns; if the true nebular light is stronger than any grid entry, the reported excess is a limitation of the grid, not a missing stellar or dust component.

Editorial extensions

If this is right

  • Ages from CIGALE for young, low-mass eYSCs are biased: a fraction of strong Pa-alpha emitters with equivalent widths pointing to ages well below 6 Myr are fitted with ages ≥6 Myr.
  • Any SED-fitting pipeline that uses deterministic, fully sampled IMFs with no pre-main-sequence stars will underestimate the 1.5–2.5 µm flux of embedded clusters and will push dust parameters to unrealistic values to compensate.
  • The Pa-alpha equivalent-width age relation is unreliable for clusters below roughly 5,000 solar masses, where stochastic sampling makes a given EW consistent with both young and old ages.
  • Adding young stellar object SEDs and stochastically sampled IMFs with pre-main-sequence emission to fitting codes is necessary to recover credible ages, masses, and dust parameters for emerging clusters.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If optically selected young clusters already show ~0.2 mag residuals, legacy HST-based cluster catalogs may carry a milder version of the same NIR bias, systematically underestimating the NIR flux of their youngest objects.
  • The paper does not test whether the excess tracks accretion; correlating the 1.5–2.5 µm residual with Br-gamma or Pa-alpha line width within the ≤3 Myr bin would separate a YSO-disk origin from a purely photospheric PMS origin.
  • Adding YSO SED templates to the fitting grid is a direct falsification test: the excess should disappear and the fitted dust parameters should return to the Umin~1–10, gamma~0.5–1 ranges expected from MIR-FIR studies.
  • Because the 3.3 µm PAH continuum subtraction assumes stellar plus nebular plus dust model continua, a missing YSO component would bias measured PAH equivalent widths, with consequences for PAH-based star-formation-rate calibrations in embedded regions.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 5 minor

Summary. The paper combines HST and JWST/NIRCam photometry to fit 0.2–5 μm SEDs of ~3800 emerging young star clusters (eYSCs) in four FEAST galaxies (M51, M83, NGC 628, NGC 4449) with CIGALE. The central empirical claim is a systematic model-observation residual at 1.5–2.5 μm (F150W and F200W), where CIGALE best-fit fluxes underestimate the observed fluxes; the residual is reported for all four galaxies and appears strongest for clusters with CIGALE-fitted ages ≤6 Myr and masses ≤3000 M⊙. The authors test and reject aperture size and dust-model choice as the origin, show that a dust-free fit up to F200W preserves the excess, and use slug stochastic IMF simulations to show that PMS stars plus extinction can partially but not fully reproduce the scatter. They conclude that current SSP-based models are missing one or more NIR ingredients, possibly YSO emission, stochastic IMF/PMS contributions, or non-homogeneous dust geometries. The paper also reports that CIGALE assigns ages ≥6 Myr to a fraction of strong Paα emitters whose Paα equivalent widths suggest younger ages.

Significance. If the central claim holds, this is an important empirical falsification test for current SED models of embedded young clusters: a reproducible 1.5–2.5 μm excess across four galaxies and hundreds to thousands of clusters would affect age/mass derivations and motivate inclusion of YSO SEDs, PMS emission, and stochastic IMF sampling in cluster SED fitting. The paper has clear strengths: the residual is quantified consistently across multiple environments; the aperture test (App. B), the dust-free test (Sec. 5.2), and the slug comparison (Sec. 5.4) are good robustness checks; and the public data products are a useful community resource. However, the headline claim that the excess is 'not accounted for by current models' is stronger than what the tested CIGALE grid demonstrates, because only a restricted nebular parameter cube is explored. In addition, the demographic statement that the excess is strongest in young, low-mass clusters is made using age and mass bins from the very fits that fail in the NIR, which introduces a partial circularity. These issues are addressable, but they are load-bearing for the paper's main conclusions.

major comments (3)
  1. [Sec. 3.1.1 / Tab. 3] The claim that the F150W/F200W excess is 'not accounted for by current stellar population models' is too strong relative to the experiments. The tested nebular grid is log U = -3.5…-2, n_e = 10, 100 cm^-3, f_esc = 0.01…0.6, f_dust = 0.01…0.3. The insensitivity test in Sec. 3.1.1 varies parameters only within these ranges; it does not establish that the ranges bracket the true nebular emission of compact, embedded, very young HII regions. At 1.5–2.5 μm, free-free and free-bound nebular continuum can be significant, and a stronger continuum than any grid point (e.g., higher n_e, very low f_esc, or different covering factor) would produce exactly this residual pattern. Please either extend the grid to physically motivated extremes (e.g., n_e up to 10^4 cm^-3, f_esc below 0.01, larger f_dust), quantify the maximal nebular contribution at F150W/F200W, or temper the Abstract/Sec. 6 wording to
  2. [Sec. 4 / Fig. 6] The statement that the NIR excess is 'most prominent in low-mass (≤3000 M⊙) and young (≤6 Myr) clusters' is based on bins of best-fit age and stellar mass from the same CIGALE fits that fail in the NIR. A missing NIR component can bias both fitted ages and masses, so the demographic conclusion is partially circular. What is robust is the direct model-observation residual itself; the dependence of that residual on fitted parameters is a secondary, model-dependent result. The Paα EW analysis in Sec. 5.6 addresses only the misclassification of the >6 Myr bin and is itself affected by excess continuum in F150W/F200W. To support the headline trend, use an independent age or mass indicator (e.g., Paα EW, HST/optical colors, or slug prior predictions), or explicitly rescale the claim to 'clusters that CIGALE classifies as young and low mass'.
  3. [Sec. 3.1.1 / Sec. 5.2] The choice of the 'adopted' dust grid is justified by lower reduced χ² rather than by physical priors, and the paper interprets the preference for low U_min / high γ as evidence of model shortcomings at 3–5 μm. Because the dust parameters are essentially unconstrained without MIR/FIR data, this preference could be a consequence of the same missing NIR component being absorbed by flexible dust templates rather than a separate physical failure. The dust-free fit in Sec. 5.2 is a good test for the 1.5–2.5 μm excess and supports that result, but it does not establish the separate claim about the dust parameter grid. I recommend presenting the dust-grid preference as a suggestive byproduct of the NIR excess, not as an independent demonstration of missing model components.
minor comments (5)
  1. [Sec. 2.2] Typographical issues to correct: 'FULLBOX 4TIGHT' appears to be a malformed dither pattern name, and 'V arun' in the author list should be 'Varun'. These do not affect the science.
  2. [Sec. 5.6 / Eq. (1)] The Paα EW formula mixes line flux and bandpass notation. Please clarify whether Fλ,line and Fλ,cont are in the same units and state how the F187N filter width (240 Å) is applied. Propagating photometric uncertainties into EW uncertainties would make the age comparison in Fig. 10 more informative.
  3. [Appendix A] The test of nebular-grid insensitivity in Appendix A is performed on optically selected YSCs in NGC 4449 using Hα, not on eYSCs in the NIR bands where the excess is found. This is a useful consistency check, but it is not equivalent to testing grid coverage at 1.5–2.5 μm for embedded clusters. The text should state this limitation explicitly.
  4. [Fig. 5 / Sec. 4] The F814W residual distribution shows a negative tail that is described only as 'the opposite behavior'. A brief quantitative statement (e.g., median Δm and fraction of objects beyond ±0.5 mag) would help the reader assess whether this is a separate model deficiency or a compensating effect of the NIR excess.
  5. [Fig. 9 / Fig. 15] The yggdrasil evolutionary track is shown as a gray line, but the caption does not state all model assumptions (e.g., f_cov = 0.5, E(B-V)=0). Adding these values to the caption would improve reproducibility.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the NIR excess is a direct data–model residual, and the paper's central claims are supported by independent checks.

full rationale

The central claim is an observational residual: m_CIG − m_obs in F150W/F200W (Sec. 4, Figs. 5–6). This residual is not an input to CIGALE; it is the output of a χ² minimization over the full 0.2–5 μm SED. The conclusion that the excess is 'not accounted for by current stellar population models' is a statement about the tested CIGALE grid, not a quantity defined to equal an input. Binning residuals by CIGALE-recovered age and mass (Fig. 6) introduces a statistical covariance between the residual and fitted parameters, and the paper acknowledges the resulting age biases; however, no equation defines the residual in terms of age/mass, and the independent Paα EW age analysis (Sec. 5.6) provides an external check that the qualitative age trend is not purely an artifact. The nebular-grid coverage (Sec. 3.1.1) is a model-completeness assumption: the paper shows insensitivity within the tested log U, n_e, f_esc, f_dust ranges but cannot prove the true eYSC nebular emission is bracketed. This is a correctness risk, not circularity. Self-citations to FEAST companion papers (Gregg et al. 2024; Pedrini et al. 2024; Knutas et al. 2025; Linden et al. in prep; Adamo et al. in prep) are used for data reduction, catalogs, and grid details that are also specified in this paper; they are not used to force the central conclusion. The slug comparison (Sec. 5.4) is a forward model, not a fit to the residuals. No load-bearing step reduces by construction to its input.

Assumptions & free parameters 2 free parameters · 4 assumptions · 0 invented entities

No new physical entities are introduced. The candidate explanations (YSO disks, PMS stars, Be/WR stars, clumpy dust, multiple bursts) are existing astrophysical components invoked from the literature (Sec. 5.4-5.5). The ledger's main debt is the adequacy of the physical model grid rather than any invented ingredient.

free parameters (2)
  • Dust grid ranges (umin, gamma) = umin: 0.3-1.0; gamma: 0.01-0.5 (AD grid)
    Chosen because they minimize reduced chi2 in CIGALE; the authors state explicitly there is no physical motivation for these ranges (Sec. 3.1.1, Fig. 2). The excess persists when dust is excluded (Sec. 5.2), so this parameter choice affects the 'model shortcoming' interpretation but not the existence of the residual.
  • Per-cluster fitted age, stellar mass, E(B-V) = Age 1-10 Myr, M* ~ 10^2-10^4 M_sun, E(B-V) medians ~0.6-0.8 mag (Fig. 3)
    CIGALE outputs used to define the age and mass bins that characterize the excess (Sec. 4). These estimates are themselves contaminated by the excess, adding a circular component to the 'young, low-mass' claim.
assumptions (4)
  • domain assumption Each eYSCI is treated as a single stellar population from one instantaneous burst of star formation.
    Sec. 3.1: 'We consider an eYSC SED to be generated by an instantaneous burst of star formation.' If many objects are complexes of sub-clusters or contain age spreads of a few Myr, the residual interpretation changes; the authors acknowledge this in Sec. 5.5.
  • domain assumption CIGALE's Bruzual & Charlot (2003) templates, with no PMS or YSO emission, adequately represent the stellar continuum.
    The excess is defined against these templates. The 'missing ingredients' conclusion depends on these templates being otherwise complete; slug with Dotter (2016) PMS tracks is the only test of PMS contribution (Sec. 5.4).
  • domain assumption The nebular emission grid (CLOUDY, Inoue 2011) with tested logU, ne, f_esc, f_dust ranges brackets the true ionized gas contribution.
    Sec. 3.1.1 asserts results are insensitive to the nebular grid, but only within the tested ranges. If the true nebular continuum at 1.5-2.5 microns lies outside this grid, the residual would be a grid-coverage artifact rather than a missing stellar ingredient.
  • domain assumption Pa-alpha equivalent width derived from F150W-F200W continuum interpolation, interpreted with yggdrasil tracks, is a valid age indicator.
    Used to argue that CIGALE wrongly assigns ages >=6 Myr to a fraction of strong Pa-alpha emitters (Sec. 5.6). The paper notes the EW is itself affected by the NIR excess and that the EW-age relation breaks down below 3000 M_sun (Fig. 11, Sec. 5.6), so this assumption carries its own caveats that the authors explicitly flag.

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Cite this review

Pith. "Pith review of The near infrared SED of young star clusters in the FEAST galaxies: Missing ingredients at 1-5 $\mu$m." pith.science (2026). https://pith.science/paper/5O3FOLJI

@misc{pith2026250901670,
  author       = {Pith},
  title        = {Pith review of: The near infrared SED of young star clusters in the FEAST galaxies: Missing ingredients at 1-5 $\mu$m},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/5O3FOLJI}},
  note         = {Machine review of arXiv:2509.01670}
}
abstract

We present a combined HST and JWST 0.2 - to - 5 $\mu$m analysis of the spectral energy distributions (SEDs) of emerging young star clusters (eYSCs) in four nearby galaxies from the Feedback in Emerging extrAgalactic Star clusTers (FEAST) survey: M51, M83, NGC 628, and NGC 4449. These clusters, selected for their bright Pa$\alpha$ and 3.3 $\mu$m polycyclic aromatic hydrocarbon (PAH) emission, are still associated to their natal gas cloud and have been largely missed in previous HST optical campaigns. We modeled their SEDs using the CIGALE fitting code and identified: i) a systematic flux excess at 1.5 - 2.5 $\mu$m that is not accounted for by current stellar population models; ii) the preference for a set of dust model parameters that is not aligned with expectations from self-consistent analyses of star-forming regions, suggesting model shortcomings also in the 3 - 5 $\mu$m. The near-infrared (NIR) excess is most prominent in low-mass ($\leq 3000$ M$_\odot$) and young ($\leq 6$ Myr) clusters. Additionally, we see that the SED fitting analysis wrongly assigns ages $\geq 6$ Myr to a fraction of strong Pa$\alpha$ emitters with equivalent widths suggestive of significantly younger ages. A parallel analysis with the slug code suggests that stochastic initial mass function (IMF) sampling of pre-main-sequence stars combined with extinction might partially reduce the gap. We conclude that the inclusion of young stellar object SEDs, along with more realistic sampling of the cluster IMF, might be needed to fully account for the stellar population and dust properties of eYSCs.

Figures

Figures reproduced from arXiv: 2509.01670 by the authors.

Figure 1
Figure 1. NIRCam detected eYSC populations in M51 (left panel), M83 (top right panel), NGC 628 (middle right panel) and NGC 4449 (bottom right panel). For each galaxy, the RGB color scheme is the following: F335M continuum subtracted map (red), F187N continuum subtracted map (green), F115W map (blue). For NGC 628, we replaced F187N with F405N, due to better visual quality of the map. We highlight the position of the eYSC popu… view at source ↗
Figure 2
Figure 2. [PITH_FULL_IMAGE:figures/full_fig_p009_2.png] view at source ↗
Figure 3
Figure 3. Normalized distributions of age, stellar mass, and E(B-V) for eYSCs in our sample of galaxies, obtained with CIGALE. We use different colors and line styles to distinguish the distributions of each galaxy. In the middle panel, we drew a dashed line at M∗ = 1000 M⊙ to guide in the plot visualization. In the right panel, we added median values of the E(B-V) distributions as vertical lines. (see Sec. 2.2). If a specifi… view at source ↗
Figures from the paper (12 more)
Figure 4
Figure 4. Figure 4: Observed SEDs, best fit models and recovered best fluxes for four representative eYSCs in M51. For each panel, the title of the plot describes the fitted properties of the specific eYSC (represented by a unique ID): χ 2 reduced, Age and stellar mass. The observed fluxe…
Figure 5
Figure 5. Figure 5: Distributions of the residuals mCIG−mobs in eight selected filters (F555W, F814W, F115W, F150W, F187N, F200W, F300M, F444W) for the sample of eYSCI in M51. For each filter, mCIG−mobs represents the difference in magnitude between the best fitted flux from the CIGALE fi…
Figure 6
Figure 6. Figure 6: Median values of the residual distributions mCIG−mobs (see [PITH_FULL_IMAGE:figures/full_fig_p013_6.png]
Figure 7
Figure 7. Figure 7: Median values of the residual distributions mCIG−mobs for eYSCI in M51, as shown in the top left panel of [PITH_FULL_IMAGE:figures/full_fig_p014_7.png]
Figure 8
Figure 8. Figure 8: Median values of the residual distributions mCIG−mobs for the optically selected YSC population in M51 younger than 10 Myr. The layout of the figure is as presented in [PITH_FULL_IMAGE:figures/full_fig_p015_8.png]
Figure 9
Figure 9. Figure 9: NIR color-color diagrams in ABmag for simulated slug cluster libraries with different fixed stellar mass and color￾coded by cluster age. The grey line represents a stellar evolutionary track computed with the yggdrasil code. Each point of the track is color-coded by ag…
Figure 10
Figure 10. Figure 10: Distribution of age differences for eYSCI in M51, M83, NGC 628 and NGC 4449, obtained using two different methods. For each panel, on the x-axis, AgeCIGALE represents the best fit values of age from CIGALE, while AgeEW is estimated from Paα EWs, as described in Sec. 5…
Figure 11
Figure 11. Figure 11: Paα EW as a function of age for simulated slug cluster libraries with different fixed stellar masses of 500, 1000, 3000 5000 and 10000 M⊙, as defined in Sec. 5.4. Each panel corresponds to a specific stellar mass, as indicated by the label. The darker lines represent …
Figure 12
Figure 12. Figure 12: Comparison between the CIGALE-estimated ages of the optical YSC population in NGC 4449 (see Sec. 2.3) and the age estimates from the LEGUS survey (Whitmore et al. 2020). In the left panel, LEGUS ages are derived using only broadband filters, while in the right panel, …
Figure 13
Figure 13. Figure 13: Same as the top right panel of [PITH_FULL_IMAGE:figures/full_fig_p022_13.png]
Figure 14
Figure 14. Figure 14: Same as [PITH_FULL_IMAGE:figures/full_fig_p023_14.png]
Figure 15
Figure 15. Figure 15: Same as [PITH_FULL_IMAGE:figures/full_fig_p023_15.png]

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