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arxiv: 2606.20979 · v1 · pith:BUOVCTTFnew · submitted 2026-06-18 · 🌌 astro-ph.GA · astro-ph.SR

Globular Clusters in the Time of the JWST. I. Survey Design and First Results on Multiple Populations and Beyond

A. P. Milone , A. F. Marino , G. Cordoni , E. Dondoglio , M. V. Legnardi , T. Ziliotto , E. Bortolan , F. Muratore
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F. D'Antona A. Renzini G. Girardi L. Gorza A. Mastrobuono-Battisti C. Ventura P. Ventura V. Altomonte L. Bisigello Y. Cavecchi F. Dell'Agli A. Dotter E. P. Lagioia C. Li S. Lionetto A. Marchuk J. Qi G. Rodrighiero M. Tailo H. Wirth
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Pith reviewed 2026-06-26 16:04 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.SR
keywords globular clustersmultiple populationsJWSTlow-mass starsmain sequencehelium abundanceM-dwarf gapproper motions
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The pith

JWST detects multiple stellar populations among low-mass stars in all eleven observed globular clusters.

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

The paper begins a uniform JWST survey of Galactic globular clusters focused on very low-mass stars, where multiple populations had been hard to study before. It reports that every one of the eleven clusters shows evidence of multiple populations in the low-mass regime through splits or spreads in the main sequence. Some clusters display discrete sequences while others show smoother distributions that track helium and oxygen variations, and one cluster reveals an M-dwarf gap matching the Jao gap seen in field stars. These results matter because low-mass stars make up most of a cluster's mass and can trace how chemical differences arose early in cluster history.

Core claim

Multiple populations are detected among low-mass stars in all eleven clusters, with discrete main sequences in NGC 288, NGC 6723, and NGC 2808, more continuous distributions in NGC 104 and the Type II clusters NGC 1851 and NGC 6656, patterns consistent with varying helium and oxygen abundances in the bulge clusters NGC 6528, NGC 6553, and NGC 6440, populations spanning different ages and helium variations within the old population of Terzan 5, and an M-dwarf gap in NGC 104 around 0.35 solar masses.

What carries the argument

Deep NIRCam infrared photometry combined with proper-motion cleaning that isolates true cluster members and exposes abundance-driven splits in the main sequence of cool, low-mass stars.

If this is right

  • Multiple populations extend to the lowest-mass stars across a wide range of cluster masses and environments.
  • Bulge clusters exhibit helium-oxygen patterns that do not scale simply with total cluster mass.
  • Terzan 5 and Liller 1 contain subpopulations with age and helium differences inside their oldest stars.
  • At least one cluster hosts an M-dwarf gap at 0.35 solar masses consistent with the Jao gap.
  • The survey supplies a homogeneous dataset for later studies of cluster evolution and Galactic populations.

Where Pith is reading between the lines

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

  • If the observed patterns hold across more clusters, they would imply that the mechanism creating multiple populations operated before the lowest-mass stars formed.
  • The bulge-cluster results could link globular-cluster chemistry directly to Milky Way bulge star-formation history.
  • Confirmation of the M-dwarf gap in additional clusters would test whether the gap is a universal feature of low-mass stellar interiors.
  • The same photometric methods could be applied to extragalactic clusters once JWST reaches comparable depths.

Load-bearing premise

The high-precision photometry and proper-motion selection cleanly separate genuine chemical differences from scatter, crowding, or field stars even at the faintest magnitudes.

What would settle it

Spectroscopic abundance measurements of individual low-mass stars in one of the clusters showing no helium or oxygen differences at the locations of the reported photometric sequences would falsify the multiple-population detection.

Figures

Figures reproduced from arXiv: 2606.20979 by A. Dotter, A. F. Marino, A. Marchuk, A. Mastrobuono-Battisti, A. P. Milone, A. Renzini, C. Li, C. Ventura, E. Bortolan, E. Dondoglio, E. P. Lagioia, F. D'Antona, F. Dell'Agli, F. Muratore, G. Cordoni, G. Girardi, G. Rodrighiero, H. Wirth, J. Qi, L. Bisigello, L. Gorza, M. Tailo, M. V. Legnardi, P. Ventura, S. Lionetto, T. Ziliotto, V. Altomonte, Y. Cavecchi.

Figure 2
Figure 2. Figure 2: shows the isochrones of 1P and 2P stars in the MF200W vs.(MF115W − MF200W) and MF277W vs.(MF277W − MF444W) CMDs (crimson and blue solid lines, respectively). We also include isochrones computed by changing only the helium abundance while keeping the C, N, and O content of 1P stars fixed (blue dashed lines), and by changing only the CNO abundances while maintaining the 1P helium content (crimson dashed line… view at source ↗
Figure 1
Figure 1. Figure 1: Top and middle panels: Ratio between synthetic spec￾tra of stars with [Fe/H]= −1.5 and 1P and 2P abundance patterns (Milone et al. 2023a). The 2P models are characterized by en￾hanced He and N abundances and depleted C and O abundances relative to their 1P counterparts. The top panel refers to bright MS stars, whereas the middle panel shows stars fainter than the MS knee. Bottom panel: Transmission curves … view at source ↗
Figure 3
Figure 3. Figure 3: CMD of NGC 2808 from short-wavelength channel photometry (left). Red error bars indicate the average photometric uncer￾tainties in colour and magnitude computed in different magnitude bins. The right panel shows a zoom of the region of the left-panel CMD around the MS knee. the target itself. The choice of N and the magnitude range was optimized to balance sensitivity to local systematics and statistical r… view at source ↗
Figure 4
Figure 4. Figure 4: mF 115W versus mF 115W − mF 200W CMDs corrected for differential reddening of stars in the fields of view of the studied GCs, sorted in alphabetical order. The average color and magnitude uncertainties, calculated for stars in different magnitude bins, as a function of magnitude are indicated by the red error bars plotted on the left side of each diagram. MNRAS 000, 1–21 (2026) [PITH_FULL_IMAGE:figures/fu… view at source ↗
Figure 5
Figure 5. Figure 5: Differential-reddening-corrected CMDs of stars in the fields of view of Terzan 5 (left) and Liller 1 (right). Left: mF115W versus mF115W − mF200W. Right: mF200W versus mF814W − mF200W. All three GCs clearly exhibit split or multiple MSs among M-dwarfs. To better highlight the presence of multiple pop￾ulations in the low-mass regime, we show in [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: mF 277W versus mF 277W − mF 444W CMDs of stars in the field of view of the studied clusters. MNRAS 000, 1–21 (2026) [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Proper motion diagrams for stars in the field of view of the studied clusters. row upper MS, whereas both NGC 6528 and NGC 6440 ex￾hibit two distinct MSs. If the observed MS splitting is driven by helium variations, these differences may indicate a smaller internal helium spread in NGC 6553 compared to NGC 6528 and NGC 6440. These findings appear to challenge previous evidence sug￾gesting that the extent o… view at source ↗
Figure 8
Figure 8. Figure 8: Illustration of the procedure adopted to select probable cluster members in NGC 2808. Left panel: mF277W magnitude as a function of the total proper motion, µR, relative to the cluster mean motion. The teal line marks the boundary between probable cluster members (black points) and field stars (teal symbols).Middle panel: mF277W vs. mF277W − mF444W CMD from long-wavelength photometry, with the same colour … view at source ↗
Figure 9
Figure 9. Figure 9: mF200W vs. mF115W − mF200W CMDs of the studies GCs, zoomed in on the MS. For NGC 2808, NGC 6553, NGC 6528, NGC 6440, and NGC 6656, which are significantly affected by field-star contamination, only proper-motion-selected probable cluster members are shown. MNRAS 000, 1–21 (2026) [PITH_FULL_IMAGE:figures/full_fig_p013_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: ChMs of M-dwarfs for the Type I GCs, NGC 288, NGC 6723, NGC 2808 and NGC 104 and for the Type II GCs NGC 1851 and NGC 6656. population, the bulk of cluster members enclosed within the crimson circle, and a kinematically cold component consis￾tent with Galactic disk stars. This latter population shows a tight, flattened distribution in proper-motion space, with µb narrowly distributed around zero. Notably,… view at source ↗
Figure 11
Figure 11. Figure 11: CMDs of proper-motion–selected stars in Terzan 5, corrected for differential reddening. The right panel shows stars at radial distances > 50′′ from the cluster center, while the bottom-middle panel presents the Hess diagram for stars above the knee. In this case, the reference frame is rotated so that the vertical axis aligns with the gray segment shown in the left panel. The top-middle panel zooms in on … view at source ↗
Figure 12
Figure 12. Figure 12: Proper-motion diagram of stars in the field of view of Liller 1 (left panel). The middle and right panels show the CMDs corresponding to stars selected in the left panel: probable cluster members within the crimson circle, and field stars within the teal rectangle, respectively. MNRAS 000, 1–21 (2026) [PITH_FULL_IMAGE:figures/full_fig_p015_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: CMD of stars with measured proper motions in the field of view of NGC 6656. Black and red symbols denote cluster members and field stars, respectively. Probable white dwarfs are marked by teal crosses. photometric diagrams for all clusters in our sample and high￾lighted the main features of their stellar populations. Building on these results, we will derive the fraction of stars belonging to 1P and 2P st… view at source ↗
Figure 14
Figure 14. Figure 14: Top panels: Hess diagram of stars fainter than the MS knee in NGC 104 (left) and corresponding luminosity func￾tion (right). Bottom panels: CMD of NGC 104. 1P stars are color￾coded according to their local density in the CMD, while all other stars are shown in gray. The right panel compares the luminos￾ity functions of all stars (gray histogram) and 1P stars (light-red histogram). In the left panels, the … view at source ↗
Figure 15
Figure 15. Figure 15: Proper-motion-selected CMDs of Bulge and field stars toward NGC 6656, corrected for differential reddening. The inset shows the histogram distribution of the stars located withing the gray dashed rectangle. The teal line is the best-fit bi-Gaussian function and its two components are represented with gray dashed lines. The right-hand panel shows 12-Gyr isochrones from the BaSTI database, overplotted for d… view at source ↗
Figure 16
Figure 16. Figure 16: Example of a background galaxy identified in the field of NGC 1851. The upper-left panel shows a three-colour composite image of a 6 × 6 arcsec region centered at RA = 05h13m45.48s , Dec = −40◦ 04′ 04.5 ′′. The upper-right panel presents the observed SED of the central red galaxy together with the best-fitting template derived using the EAZY code. The bottom panels display the stacked images in the F444W,… view at source ↗
Figure 17
Figure 17. Figure 17: Candidate LRD in the field of NGC 1851. Same format as [PITH_FULL_IMAGE:figures/full_fig_p020_17.png] view at source ↗
read the original abstract

Globular clusters (GCs) host multiple stellar populations with distinct chemical compositions, but their properties among very low-mass stars remain poorly constrained. The James Webb Space Telescope (JWST) enables precise infrared studies that are highly sensitive to abundance variations in cool stars. We initiate a homogeneous survey of Galactic GCs, based primarily on deep JWST GO-8960 observations and complemented by archival JWST and Hubble Space Telescope data, to characterize multiple populations across a wide range of cluster properties. In this first paper, we present the survey and initial NIRCam results. We analyze eleven GCs, deriving high-precision photometry and astrometry to measure proper motions. Multiple populations are detected among low-mass stars in all clusters, with diverse behaviors. We find discrete main sequences in NGC 288, NGC 6723, and NGC 2808, and more continuous distributions in NGC 104 and the Type II clusters NGC 1851 and NGC 6656. The bulge clusters NGC 6528, NGC 6553, and NGC 6440 show patterns consistent with varying helium and oxygen abundances that do not scale simply with cluster mass. In Terzan 5 and Liller 1, we identify populations spanning different ages and helium variations within the old population of Terzan 5. We also detect an M-dwarf gap in NGC 104 around 0.35 solar masses, consistent with the Jao Gap of field stars and open clusters. This work establishes the foundation for a homogeneous JWST survey of Galactic GCs and provides a valuable dataset for studies of cluster evolution, Galactic stellar populations, and background extragalactic sources.

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 / 0 minor

Summary. The paper presents the design of a homogeneous JWST survey of Galactic globular clusters and reports initial NIRCam photometry and proper-motion results for eleven clusters. It claims detections of multiple populations among low-mass stars in all eleven, with discrete main sequences in NGC 288, NGC 6723 and NGC 2808, more continuous distributions in NGC 104 and the Type II clusters NGC 1851 and NGC 6656, helium/oxygen patterns in the bulge clusters NGC 6528, NGC 6553 and NGC 6440, age and helium variations in Terzan 5 and Liller 1, and an M-dwarf gap in NGC 104 around 0.35 solar masses.

Significance. If the photometric and astrometric cleaning procedures prove robust, the work supplies the first homogeneous JWST dataset on multiple populations at low masses, where infrared sensitivity to abundance variations is high. The survey design, use of public GO-8960 and archival data, and the reported M-dwarf gap (linking to the Jao Gap) are concrete strengths that would enable future comparative studies of cluster evolution and Galactic populations.

major comments (2)
  1. [Abstract and §2 (Survey Design)] The abstract and survey description state clear detections across all eleven clusters but supply no quantitative metrics (e.g., sequence separation in magnitudes, photometric error distributions, or membership probability thresholds). Without these, it is impossible to assess whether the reported discrete versus continuous distributions exceed residual crowding or field contamination in the faint regime.
  2. [§3 (Data Analysis) and Results paragraphs on NGC 288, NGC 6723, NGC 2808] The central claim that NIRCam photometry plus proper-motion cleaning isolates genuine low-mass multiple-population signals rests on the untested assumption that chosen PM thresholds and crowding corrections suppress systematics below the observed separations. No error budget, artificial-star tests, or residual-contamination simulations are referenced for the low-mass regime.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed comments. We agree that additional quantitative metrics and validation details will strengthen the manuscript and will incorporate them in the revision.

read point-by-point responses

  1. Referee: [Abstract and §2 (Survey Design)] The abstract and survey description state clear detections across all eleven clusters but supply no quantitative metrics (e.g., sequence separation in magnitudes, photometric error distributions, or membership probability thresholds). Without these, it is impossible to assess whether the reported discrete versus continuous distributions exceed residual crowding or field contamination in the faint regime.

    Authors: We acknowledge the absence of explicit quantitative metrics in the abstract and §2. In the revised manuscript we will add a summary of photometric error distributions at the faint end, measured sequence separations (in color and magnitude), and the precise proper-motion membership probability thresholds (typically >0.75 after outlier rejection) used for each cluster. These values will be placed in §2 with a brief reference in the abstract, enabling direct evaluation of the separations relative to errors and contamination. revision: yes

  2. Referee: [§3 (Data Analysis) and Results paragraphs on NGC 288, NGC 6723, NGC 2808] The central claim that NIRCam photometry plus proper-motion cleaning isolates genuine low-mass multiple-population signals rests on the untested assumption that chosen PM thresholds and crowding corrections suppress systematics below the observed separations. No error budget, artificial-star tests, or residual-contamination simulations are referenced for the low-mass regime.

    Authors: Section 3 describes the PM cleaning and crowding corrections, but we agree that an explicit error budget and validation tests for the low-mass regime are not referenced. We will expand §3 to include (i) a tabulated error budget combining photometric uncertainties and crowding, (ii) results from artificial-star tests quantifying recovery rates and bias at the faint end, and (iii) residual-contamination simulations after applying the adopted PM thresholds. These additions will demonstrate that the observed separations in NGC 288, NGC 6723, and NGC 2808 exceed the quantified systematics. revision: yes

Circularity Check

0 steps flagged

No circularity: observational detections from JWST photometry

full rationale

The paper presents a survey and reports direct detections of multiple populations via NIRCam photometry and proper-motion cleaning in eleven globular clusters. Central claims rest on observed sequences in color-magnitude diagrams without any derivation chain, fitted parameters, equations, or self-citation load-bearing steps. The work is self-contained data analysis against external photometric benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Observational survey paper; no new theoretical parameters, axioms, or invented entities are introduced. The work relies on standard assumptions of stellar photometry and proper-motion membership that are inherited from prior literature.

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Reference graph

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