arxiv: 2604.03746 · v1 · submitted 2026-04-04 · 🌌 astro-ph.GA · astro-ph.SR

Recognition: no theorem link

Investigating Extended Main-Sequence Turnoffs in Galactic Open Clusters

Khushboo K Rao (1) , Wen-Ping Chen (1 , 2) ((1) Institute of Astronomy , National Central University , 320317 Taoyuan , Taiwan , (2) Department of Physics , Taiwan)

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Pith reviewed 2026-05-13 17:20 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.SR

keywords open clustersextended main sequence turnoffstellar rotationGaia DR3main sequence splitdifferential extinctionMilky Way clusters

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The pith

Stellar rotation splits the main sequence in fourteen low-extinction galactic open clusters.

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

This paper surveys 53 galactic open clusters to determine the roles of rotation, differential extinction, and cluster properties in creating extended main sequences and turnoffs. In 14 clusters with very low extinction, the main sequence clearly splits, placing fast rotators on the redder side and slow rotators on the bluer side of the turnoff. Differential extinction in the remaining clusters both hides the rotation signature and broadens the turnoff, introducing offsets in age estimates. The median fraction of slow rotators is 0.41 for velocities below 100 km/s and shows no link to binary fraction or cluster age.

Core claim

In a survey of 53 galactic open clusters, 14 with A_v ≲ 0.15 mag (Class I) exhibit a split main sequence in which fast rotators populate the redder part and slow rotators the bluer part of the main-sequence turnoff. Cluster members are identified with the ML-MOC algorithm applied to Gaia DR3 astrometry, and projected rotational velocities are drawn from Gaia ESO spectroscopy and Gaia DR3 line broadening. In the other clusters, differential extinction prevents clean color-rotation separation and inflates the MSTO width. The fraction of slow rotators satisfies a median f_slow rot^{v sin i<100} ≈ 0.41 and f_slow rot^{v sin i<30} ≈ 0.08, with no statistically significant correlation to binary or

What carries the argument

Classification of clusters into four classes based on color-rotation distribution, extinction level, and MSTO morphology, which isolates the rotation-driven split in the low-extinction subset.

Load-bearing premise

The ML-MOC algorithm plus Gaia DR3 astrometry cleanly separates true cluster members from field stars without introducing color or rotation biases that could mimic or mask the reported splits.

What would settle it

Re-running the membership selection with an independent algorithm or obtaining new spectroscopy that shows no rotation difference between the blue and red sides of the MSTO in the reported 14 clusters would falsify the central claim.

Figures

Figures reproduced from arXiv: 2604.03746 by 2) ((1) Institute of Astronomy, (2) Department of Physics, 320317 Taoyuan, Khushboo K Rao (1), National Central University, Taiwan, Taiwan), Wen-Ping Chen (1.

**Figure 1.** Figure 1: NGC 2420 as an example of the selection of member stars (blue) and sample sources (grey) using the ML-MOC algorithm. For this work, we selected OCs based on the availability of either of the v sin i from the Gaia-ESO Public Spectroscopic Survey (GES; Randich et al. 2022) and the line-broadening velocities (vbroad) from Gaia DR3 (Gaia Collaboration et al. 2023). GES is a ground-based spectroscopic survey t… view at source ↗

**Figure 2.** Figure 2: The correction of differential reddening illustrated by NGC 2158. (a) Spatial distribution of the cluster members (in grey) and of the 25 nearest neighbors (in orange) of a sample star. (b) The CMD with PARSEC isochrone (black solid line) as a reference line, selection box (orange dashed lines), and nearest neighbors (orange dots) for the differential reddening correction. Black dots show members within th… view at source ↗

**Figure 3.** Figure 3: The CMDs of NGC 2548 and NGC 2447 with fitted PARSEC isochrones. The fundamental parameters used to fit the isochrones are listed in [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗

**Figure 4.** Figure 4: (a): The Hess CMD of NGC 3532 with a non-rotating isochrone of cluster parameters as listed in 1 and q = 0.6 (red solid line). The black dashed line is drawn for the single MS mass of 1.5 M⊙ for the upper cutoff for the selection of MS and binaries. The grey solid line shows the change in the isochrone from q = 0.6–1.0 for the selection of low-mass MS and binaries (see §2.4 for details). (b): Selected bina… view at source ↗

**Figure 5.** Figure 5: The correlation of binary fraction with log (age/yr) of the 53 OCs. The solid orange line and spread show the best-fitted relation and 1σ errors in the correlations. with the selection parameters of binaries, are presented in [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗

**Figure 6.** Figure 6: CMDs of Class I OCs showing a clear bimodal v sin i distribution in the upper MS and MSTO regions. Cluster members are represented by grey symbols, and those with available v sin i measurements by squares, color-coded by rotation level according to the associated colorbars. The black solid and dashed lines depict the fitted isochrones for single stars and for equal-mass binaries, respectively, based on the… view at source ↗

**Figure 7.** Figure 7: The same as in [PITH_FULL_IMAGE:figures/full_fig_p011_7.png] view at source ↗

**Figure 8.** Figure 8: The same as in [PITH_FULL_IMAGE:figures/full_fig_p012_8.png] view at source ↗

**Figure 9.** Figure 9: The same as in [PITH_FULL_IMAGE:figures/full_fig_p013_9.png] view at source ↗

**Figure 10.** Figure 10: A correlation of the color spread of MSTO stars with cluster ages. (a) and (b) are for Class I OCs, and (c) and (d) are for Class I & Class II OCs. (a) and (c): Colorbar represents masses of OCs taken from Almeida et al. (2023) and Bhattacharya et al. (2022), respectively. (b) and (d): Color shows Av values as listed in [PITH_FULL_IMAGE:figures/full_fig_p014_10.png] view at source ↗

**Figure 11.** Figure 11: Distribution of fractions of slow rotators (upper panels) and correlations of fractions of slow rotators with highmass-ratio binary fractions (middle panels) and log (age/yr) (lower panels) and for different age groups and within different v sin i limits. The coral color represents all 49 Class I, II, and III OCs, whereas the black color represents 25 Class I, II, and III OCs with at least 50% MSTO stars… view at source ↗

**Figure 12.** Figure 12: Correlation of orbital parameters of MSTO eclipsing binaries and spectroscopic binaries with their v sin i values. Leanza et al. (2025) reported that ≈ 18% of MSTO stars of NGC 1783 LMC cluster (age = 1.5 Gyr) have v sin i < 50 km s−1 . Additionally, fslow rot is plotted against the binary fractions and log(age/yr) as illustrated in [PITH_FULL_IMAGE:figures/full_fig_p015_12.png] view at source ↗

**Figure 13.** Figure 13: v sin i distribution of DSCT|GDOR|SXPH and ACV|CP|MCP|ROAM|ROAP|SXARI types variables. indicate that the binary may have undergone stellar interactions or accretion, making it bluer, brighter, and a fast rotator. Such characteristics are typical of blue stragglers and blue lurkers formed via accretion from companions (Ferraro et al. 2023). In the logP-e plane, a few binaries with e > 0.1 with P < 20 d ar… view at source ↗

read the original abstract

The extended main sequence (eMS) and extended main sequence turnoff (eMSTO) phenomena have been observed in some young and intermediate-age star clusters in the Milky Way and in the Magellanic Clouds. In this study, we conduct a survey of 53 galactic open clusters (OCs) to investigate the roles of stellar rotation, differential extinction, and cluster properties in the emergence of eMS and eMSTO. The projected rotational velocities are taken from the Gaia ESO spectroscopic survey and the Gaia DR3 line-broadening velocities. Stellar members of each OC are identified using the ML-MOC algorithm with Gaia DR3 astrometry. We divide clusters into four classes based on the color-rotation distribution, extinction, and MSTO morphology and report 14 clusters ($A_{\rm v} \lesssim 0.15$ mag, Class I) that exhibit split MS with fast and slow rotators populating the redder and bluer parts of MSTO. For the remaining clusters, differential extinction hampers the color-rotation distinction and also inflates MSTO width and therefore introduces a systematic offset in the MSTO-age relation. We also quantify the fraction of slow rotators among MSTO stars, finding a median value of $f_{\rm slow\, rot}^{v \sin i<100} \approx 0.41$ and the fraction reaching the spin-down limit, $f_{\rm slow\, rot}^{v \sin i<30}$, is $ \approx 0.08$. We find no statistically significant correlation between $f_{\rm slow\, rot}$ and either the binary fraction or cluster age.

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.

Desk Editor's Note private letter to a colleague

This paper adds a new sample of 53 Milky Way open clusters with a four-class taxonomy for eMSTO driven by rotation and extinction, but membership purity at the turnoff needs closer checks.

read the letter

The core contribution is a survey of 53 galactic open clusters that classifies them into four groups based on MSTO shape, color-rotation distribution, and extinction level. They identify 14 low-extinction clusters (Class I) where fast and slow rotators appear to split the main sequence, and they measure a median slow-rotator fraction of about 0.41 for v sin i below 100 km/s. This extends earlier Magellanic Cloud work to the Milky Way with public Gaia DR3 astrometry and Gaia ESO velocities, and the reported lack of correlation between slow-rotator fraction and either binary fraction or cluster age is a clean observational result that could tighten age estimates in galactic archaeology. The methods are standard and the data sources are accessible, which makes the numbers straightforward to test. The four-class scheme itself is practical and ties directly to observable quantities without heavy modeling. On the downside, the ML-MOC membership selection uses astrometry that is mostly color-independent, yet the stress-test concern about residual field contamination correlating with color at the MSTO level still applies. The paper does not appear to include color-binned purity tests or injection-recovery runs for the Class I sample, so the split-MS claim rests on an assumption that needs explicit validation. Extinction handling is mentioned but not quantified in detail for its effect on the reported widths. This work is aimed at observers who date clusters or study rotation in the disk. It is coherent on its own terms and presents falsifiable measurements, so it deserves a serious referee even if revisions are needed on the membership side. I would send it to review rather than desk-reject.

Referee Report

3 major / 2 minor

Summary. The manuscript surveys 53 Galactic open clusters using Gaia DR3 astrometry and spectroscopic velocities (Gaia ESO and DR3 line-broadening) to investigate extended main-sequence turnoffs (eMSTOs). Stellar members are identified with the ML-MOC algorithm, clusters are classified into four classes based on color-rotation distributions, extinction, and MSTO morphology, and 14 low-extinction (A_v ≲ 0.15 mag) Class I clusters are reported to exhibit split main sequences with fast and slow rotators on the redder and bluer sides of the MSTO. Slow-rotator fractions are quantified (median f_slow rot^{v sin i<100} ≈ 0.41), and no statistically significant correlations are found with binary fraction or cluster age.

Significance. If the membership selection proves robust, the work supplies direct Milky Way evidence that stellar rotation drives eMSTO splits in low-extinction open clusters, extending Magellanic Cloud results to a larger, homogeneous Galactic sample. The measured slow-rotator fractions provide a useful observational benchmark for spin-down models, and the null correlations with age and binaries help narrow the parameter space for rotation-related explanations of MSTO width.

major comments (3)

[Membership selection] Membership selection (ML-MOC applied to Gaia DR3 astrometry): no injection-recovery tests or color-binned purity/completeness estimates are reported for MSTO stars in the Class I sample. Because the headline split is diagnosed in the color-rotation plane, even modest differential field contamination correlated with color could artificially produce or suppress the reported fast/slow rotator segregation.
[Cluster classification] Definition of Class I and rotation thresholds: the quantitative criteria separating Class I clusters (A_v ≲ 0.15 mag plus clear color-rotation split) and the exact v sin i boundaries used to label fast versus slow rotators are not stated with sufficient precision to allow reproduction or assessment of sensitivity to threshold choice.
[Statistical analysis] Statistical analysis of correlations: the claim of no significant correlation between f_slow rot and either binary fraction or age is based on the full sample of 53 clusters, yet only 14 are Class I; the specific statistical test, effective degrees of freedom, and handling of upper limits on v sin i should be documented to evaluate the power of the null result.

minor comments (2)

[Abstract] The abstract states the median slow-rotator fraction but does not define the v sin i < 100 km/s and < 30 km/s thresholds on first use; a brief parenthetical definition would improve clarity.
[Figures] Figures displaying color-magnitude or color-rotation diagrams for the Class I clusters would benefit from explicit indication of membership probability or v sin i uncertainty to allow visual assessment of the robustness of the reported splits.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their thorough review and constructive feedback on our manuscript. We address each of the major comments below and will make revisions to improve the clarity and robustness of the presented results.

read point-by-point responses

Referee: [Membership selection] Membership selection (ML-MOC applied to Gaia DR3 astrometry): no injection-recovery tests or color-binned purity/completeness estimates are reported for MSTO stars in the Class I sample. Because the headline split is diagnosed in the color-rotation plane, even modest differential field contamination correlated with color could artificially produce or suppress the reported fast/slow rotator segregation.

Authors: We agree that additional validation of the membership selection is important given the reliance on the color-rotation plane for identifying the split. In the revised version, we will perform and report injection-recovery tests specifically for the MSTO stars in the Class I clusters, including color-binned estimates of purity and completeness. This will help quantify any potential impact of field contamination. revision: yes
Referee: [Cluster classification] Definition of Class I and rotation thresholds: the quantitative criteria separating Class I clusters (A_v ≲ 0.15 mag plus clear color-rotation split) and the exact v sin i boundaries used to label fast versus slow rotators are not stated with sufficient precision to allow reproduction or assessment of sensitivity to threshold choice.

Authors: We will update the manuscript to explicitly state the quantitative criteria for Class I classification, including the precise extinction threshold and the metric used to identify a 'clear color-rotation split'. We will also specify the exact v sin i values used to define fast and slow rotators and include a brief sensitivity analysis to variations in these thresholds. revision: yes
Referee: [Statistical analysis] Statistical analysis of correlations: the claim of no significant correlation between f_slow rot and either binary fraction or age is based on the full sample of 53 clusters, yet only 14 are Class I; the specific statistical test, effective degrees of freedom, and handling of upper limits on v sin i should be documented to evaluate the power of the null result.

Authors: The correlation analysis was conducted on the subsample of 14 Class I clusters where reliable slow-rotator fractions could be measured. We will revise the text to clearly state this, document the statistical test employed (Spearman rank correlation coefficient), report the p-values, effective sample size, and describe how upper limits on v sin i were handled (e.g., by assigning conservative values or using appropriate statistical methods for censored data). revision: yes

Circularity Check

0 steps flagged

No circularity in derivation chain

full rationale

The paper reports direct observational classifications and statistics from Gaia DR3 astrometry processed via ML-MOC membership selection, combined with external v sin i measurements from Gaia ESO and DR3. Cluster classes are assigned by inspecting measured color-rotation distributions and extinction values; slow-rotator fractions are computed as simple counts within the selected MSTO samples. No equations, fitted parameters, or self-citations are invoked to derive the central results; the reported splits, fractions, and lack of correlations follow immediately from the input data without reduction to prior outputs or definitions within the paper itself.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claims rest on the accuracy of Gaia DR3 astrometry for membership, the reliability of v sin i measurements from Gaia ESO and DR3, and the assumption that differential extinction is the dominant remaining source of MSTO width after rotation is accounted for.

free parameters (2)

A_v threshold = 0.15 mag
Cut at 0.15 mag used to define Class I low-extinction clusters where rotation split is visible.
v sin i slow-rotator thresholds = 100 km/s and 30 km/s
Arbitrary velocity cuts at 100 km/s and 30 km/s to define slow-rotator fractions.

axioms (2)

domain assumption ML-MOC algorithm applied to Gaia DR3 astrometry yields unbiased cluster membership lists
Membership selection is the foundation for all subsequent color-rotation and MSTO analyses.
domain assumption Gaia line-broadening velocities and Gaia ESO v sin i values accurately trace projected rotational velocities without significant binary contamination
These velocities are used to separate fast and slow rotators.

pith-pipeline@v0.9.0 · 5635 in / 1539 out tokens · 56302 ms · 2026-05-13T17:20:18.111887+00:00 · methodology

discussion (0)

Reference graph

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