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The impact of stellar rotations and binaries on the shape of upper main sequence near turn off in open cluster NGC\,6067

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Pith's one-line read This paper argues that the extended main-sequence turn-off in open cluster NGC 6067 is caused by a spread in stellar rotation rates, with fast rotators appearing redder and concentrated toward the cluster center, and that…

desk verdict Useful new v sini data for NGC 6067, but the headline rotation-color correlation is built on excluding seven red slow rotators without evidence, and that exclusion is load-bearing for the paper's main claim. read the letter →

arxiv 2507.14433 v1 pith:EISFO54X submitted 2025-07-19 astro-ph.SR astro-ph.GA

Jayanand Maurya , Yu Zhang , Sebastian Kamann , Hubiao Niu , Yves Frémat , Kaixiang Lang , Y. C. Joshi , M. R. Samal
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Peter De Cat Ali Esamdin
This is my paper · ORCID
classification astro-ph.SRastro-ph.GA
keywords openstarclustersstellarrotationextendedmain-sequenceturn-offstar-diskinteractiontidallockingspectroscopicbinariesvsiniNGC6067
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

The paper sets out to explain why the upper main sequence of the open cluster NGC 6067 is visibly broadened just below the turn-off, an extended main-sequence turn-off (eMSTO). Using Gaia-ESO spectra for 41 of the 280 eMSTO stars, the authors measure projected rotation velocities and find that redder eMSTO stars rotate faster, with a correlation coefficient of 0.506 and p = 0.004. They argue that this color-rotation link is best explained by gravity darkening, and that the spread in rotation itself is what produces the eMSTO. Because red fast rotators are concentrated toward the cluster center while blue slow rotators sit farther out, the authors conclude that tidal locking in close binaries is unlikely to be the cause of the rotation spread. They propose instead that star-disk interactions during the pre-main-sequence phase set the rotation rates, with central stars losing their disks earlier and therefore spinning up faster.

What carries the argument

The load-bearing measurement is the projected rotational velocity v sini, obtained by fitting synthetic spectra to Gaia-ESO spectra of eMSTO members. The argument then runs through two further devices: the fiducial-line pseudo-color separating blue (bMS) from red (rMS) parts of the eMSTO, and cumulative radial distributions with a Kolmogorov-Smirnov test (statistic 0.2609, p = 0.0001) comparing where the two groups live. A synchronization-time formula from Hurley et al. (2002) is used to show that close binaries in the cluster would be tidally locked, making the spatial distribution the decisive test between binary braking and star-disk interaction.

What would settle it

Measure v sini for every one of the 280 eMSTO members rather than only the 41 with public spectra, and recompute the cumulative radial distributions; if the red fast rotators are not actually more concentrated in the core once the full population is sampled, the star-disk interaction conclusion fails. A second check would be to measure the binary fraction separately for blue and red eMSTO stars; if blue stars turn out to have substantially more binaries, tidal locking would re-emerge as a viable cause.

Watch

Extended reading notes

Core claim

The central claim is that the observed eMSTO in NGC 6067 is a rotation effect, not an age spread or a binary artifact. The paper shows a positive correlation between v sini and color offset from the main-sequence fiducial line, with bluer-side eMSTO stars averaging about 146 km/s and redder-side eMSTO stars averaging about 247 km/s. Four double-lined spectroscopic binaries all have slowly rotating components, consistent with tidal locking, but the red fast rotators are more centrally concentrated than the blue slow rotators, contrary to what mass segregation of tidally locked binaries would predict. The authors therefore conclude that star-disk interactions in the pre-main-sequence phase, modulated by the cluster environment, produced the rotation spread and hence the eMSTO.

Load-bearing premise

The load-bearing premise is that the bluer-side and redder-side groups chosen by color are faithful stand-ins for slow and fast rotation across the whole turn-off population; with spectra for only 41 of the 280 stars, the central-versus-outskirt pattern of the unsampled majority is inferred, not measured.

Editorial extensions

If this is right

  • If the central claim is right, the eMSTO of NGC 6067 is not evidence of extended star formation or a significant binary population; it is a rotation phenomenon.
  • Gravity darkening is implicated as the physical link: fast rotators appear slightly redder and fainter at the same mass, which is why they occupy the red side of the main sequence.
  • Tidal locking is not the main brake on eMSTO rotation in this cluster; the four SB2 binaries, though slow-rotating, are too few to explain the blue population.
  • The spatial pattern, with red fast rotators in the center, matches the star-disk interaction scenario, where central stars lose their disks earlier to photoevaporation and dynamical encounters and spin up.
  • The disappearance of fast rotators below about 1.6 solar masses is consistent with magnetic braking setting in for lower-mass stars, so the rotation-spread explanation only applies to the upper main sequence.

Reading between the lines

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

  • A direct extension would be to measure v sini for all 280 eMSTO members; if the central concentration of fast rotators survives a complete sample, the star-disk interaction interpretation is on much firmer ground.
  • If the environment controls disk lifetimes, then clusters with denser cores or stronger ultraviolet fields should show a larger eMSTO width and a stronger center-versus-outskirts contrast; this cross-cluster prediction is not made explicitly in the paper.
  • Because v sini collapses true rotation onto the line of sight, the paper's rotation-color correlation may underestimate the real spread in equatorial velocities; a statistically deprojected sample could separate the gravity-darkening signal from inclination effects.
  • Applying the same analysis to a cluster of similar age but lower metallicity would test whether the rotation-spread mechanism scales with metallicity, as rotational evolution models predict.
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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 analyzes the extended main-sequence turn-off (eMSTO) in the open cluster NGC 6067 using Gaia DR3 astrometry/photometry and Gaia-ESO spectroscopy. The authors derive projected rotational velocities for 41 eMSTO stars, identify two Be stars and four SB2 binaries, and report a positive correlation between v sin i and color (r = 0.506, p = 0.004) after excluding seven slow-rotating red stars. They split the eMSTO into bluer (bMS) and redder (rMS) groups, report mean v sin i values of 146 km/s and 247 km/s respectively, and find that rMS stars are more centrally concentrated than bMS stars (K-S p = 0.0001). On this basis they argue against tidal locking in binaries as the main cause of the rotation spread and propose instead that pre-main-sequence star-disk interactions produced the spread, with the eMSTO itself arising from the rotation spread.

Significance. If the central correlation and the spatial segregation result are robust, the paper would provide an interesting new datapoint in the debate over the origin of eMSTOs, supporting the rotation-spread scenario and an environmental, pre-main-sequence origin. The study uses standard and mostly appropriate methods: Gaia-ESO spectra, synthetic spectral fitting, differential reddening correction, SB2 decomposition with GIRFIT, and a synchronization-time calculation. The paper also usefully presents quantitative measurements for a cluster with known Be stars and SB2 systems. However, the headline statistical claim rests on a post-hoc exclusion of the most inconvenient data points, and the spatial argument extrapolates from a small spectroscopic subsample to the full photometric eMSTO population; both points need substantial additional support before the conclusions can be accepted.

major comments (3)
  1. [Section 5.1, Figure 11] The central correlation (r = 0.506, p = 0.004) is computed after excluding seven eMSTO stars (IDs 21, 229, 317, 358, 403, 797, 807) with v sin i < 50 km/s on the red side, and the only stated justification is that they 'could be binaries undetectable from the current set of spectroscopic data.' No radial-velocity variability, RUWE, or other independent binarity evidence is presented for these stars. Because these seven points are the most direct counterexamples to the claimed monotonic v sin i-color relation, the reported correlation is not robust as presented. A simple inclusion of these stars in the rMS sample lowers the rMS mean from roughly 247 km/s to roughly 185 km/s, approaching the bMS mean of 146 km/s, and the reported p-value will degrade correspondingly. The authors should show that the correlation and the bMS/rMS comparison survive inclusion of these stars, or provide independent evidence that they are binaries and quantify the unresolved-binary contribution to the eMSTO width.
  2. [Section 5.2, Figure 14] The spatial argument treats the photometrically defined bMS and rMS samples as faithful proxies for slow and fast rotation across the entire eMSTO population, but v sin i is measured for only 41 of the 280 eMSTO stars (23 bMS and 18 rMS). The density contours and the K-S test in Figures 14 and 15 use all 280 stars, so the central concentration of rMS stars is not a measured central concentration of fast rotators. If the unsampled majority has a different rotation distribution, the inference that fast rotators are centrally concentrated, and hence the star-disk interaction conclusion, would be weakened. The authors should either measure rotational velocities for a substantially larger subsample or model the selection function and demonstrate that the unsampled stars cannot change the conclusion.
  3. [Section 5.2 and Table 4] The argument against tidal locking is internally inconsistent with the paper's own binary detections. The text assumes that if tidal locking were responsible for the slow-rotating eMSTO population, then the bMS population would consist of the tidally locked binaries and should be centrally concentrated. However, the four detected SB2 systems (IDs 70, 609, 643, 691) all have component v sin i values below 20 km/s and are stated to occupy the red part of the eMSTO. Thus the observed central concentration of rMS stars could instead be interpreted as a central concentration of tidally locked slow rotators, which would support rather than exclude the tidal-locking mechanism. The rejection of tidal locking needs to be reformulated using the actual colors and locations of spectroscopically confirmed slow rotators, not an assumed association between bMS stars and tidally locked binaries.
minor comments (5)
  1. [Section 3.1] The removal of nine outlier stars is described only as 'significantly deviating from the MS in visual inspection'; please provide quantitative selection criteria or show the removed stars explicitly in the CMD.
  2. [Table 3] The [Fe/H] entry for star ID 717 is printed as '-0.13+-0.05' and should be formatted consistently with the other uncertainties.
  3. [Figure 11] The horizontal axis label reads 'GBP - GRP (mag)' while the text and caption define the abscissa as the pseudo-color Delta(GBP-GRP); the label should be changed to match the quantity actually plotted.
  4. [Section 4.4, Table 4] The SB2 components have radial velocities that differ from the cluster mean of about -38.8 km/s by tens of km/s; one or two sentences explaining why these systems are still considered cluster members would help the reader.
  5. [Section 5.2] The K-S test result for the bMS and rMS radial distributions would be easier to interpret if the sample sizes entering the test were stated in the text or figure caption.

Circularity Check

0 steps flagged · score 2.0 of 10

No load-bearing circularity: the v sini-color correlation, bMS/rMS group means, and spatial K-S test are based on independent Gaia photometry and Gaia-ESO spectra, with only minor non-load-bearing self-citations.

full rationale

The central derivation chain is not circular in the technical sense. The v sini values come from Gaia-ESO spectra and the colors from Gaia DR3; the two are independent measurements. The positive correlation in Figure 11 is computed after excluding seven stars with v sini < 50 km/s, and the paper speculates that they 'could be binaries undetectable from the current set of spectroscopic data.' This exclusion is a data-robustness choice, not a definitional construction: the paper's own bMS/rMS statistics (23 bMS and 18 rMS stars, with the 14 non-SB2 rMS stars averaging 247 ± 8 km/s) imply that the seven slow stars are not part of the rMS fast-rotator sample, so including them would mainly add blue-side slow rotators and would not erase the signal. The spatial conclusion rests on the photometric K-S test (p = 0.0001) between bMS and rMS radial distributions, which is independent of the v sini fitting. The SDI explanation is imported from prior literature (Bastian et al. 2020) and tested against the new spatial data, not derived from the model's own assumptions. The self-citations to Maurya et al. (2023, 2024) are methodological or bibliographic and are not load-bearing; no uniqueness theorem or ansatz is smuggled through them. The paper also explicitly acknowledges the unresolved-binary caveat ('we cannot completely rule out the contribution of the photometrically unresolved binaries in broadening the upper MS'), which is a limitation for the interpretation but not a circular dependency. Overall, the empirical content is self-contained and externally anchored, so the circularity score is low rather than elevated.

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

The central claim rests on standard stellar and spectral models, a representative-sampling assumption for the 41 observed eMSTO stars, a dynamical expectation about mass segregation of binaries, and the prior SDI model. No new physical entities or constants are introduced, but four hand-chosen analysis parameters shape the result.

free parameters (4)
  • eMSTO selection box = G = 9.85 to 14.05 mag; G_BP-G_RP = 0.20 to 0.70 mag
    Hand-selected rectangular region in the CMD defining the 280 eMSTO stars analyzed; Section 3.1 and Figure 2.
  • Outlier exclusion threshold = v sini < 50 km/s
    Seven slow-rotating eMSTO stars are excluded from the vsini-color regression in Figure 11, with the speculation that they are undetected binaries; Section 5.1.
  • Fiducial line and reddening reference cuts = 0.5 mag magnitude bins; 80th percentile distance cut; reference magnitude range G = 14.1 to 16.1
    These choices define the bMS/rMS split and the differential reddening correction, which underpin the spatial distribution argument; Sections 3.2 and 5.1.
  • Isochrone age and mass scale = log(age) = 7.96 (91 Myr); masses 2.1 to 5.3 Msun
    Fitted with Marigo et al. (2017) isochrones at fixed AV = 0.99 from Hunt & Reffert (2023) and Z = 0.02; it sets which stars belong to the eMSTO and their masses; Section 3.1.
assumptions (4)
  • domain assumption Standard stellar models (Marigo isochrones, ATLAS9 atmospheres, SPECTRUM) accurately represent NGC 6067 stars
    Used for age, mass, Teff, log g, and vsini determinations; Sections 3.1 and 4.
  • domain assumption The 41 eMSTO stars with spectra are representative of the 280 eMSTO stars in the spatial distribution argument
    The bMS/rMS rotation characterization is based on 23 bMS and 18 rMS stars with vsini, then assumed to hold for the full color-selected samples; Section 5.2 and Figures 14-15.
  • domain assumption Tidally locked binaries, if present in the eMSTO, would be preferentially centrally concentrated due to mass segregation
    This expectation drives the rejection of the tidal-locking explanation; Section 5.2 relies on the Spitzer & Hart (1971) relaxation time and the measured weak mass segregation (MSR = 1.2).
  • domain assumption The star-disk interaction model of Bastian et al. (2020) applies to NGC 6067 and predicts faster disk dissipation in the cluster center
    The SDI mechanism is imported from prior literature and used to interpret the observed central concentration of fast rotators; Section 5.3.

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Pith. "Pith review of The impact of stellar rotations and binaries on the shape of upper main sequence near turn off in open cluster NGC\,6067." pith.science (2026). https://pith.science/paper/EISFO54X

@misc{pith2026250714433,
  author       = {Pith},
  title        = {Pith review of: The impact of stellar rotations and binaries on the shape of upper main sequence near turn off in open cluster NGC\,6067},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/EISFO54X}},
  note         = {Machine review of arXiv:2507.14433}
}
read the original abstract

We present the analysis of the extended Main Sequence Turn-Off (eMSTO) in the open cluster NGC\,6067. We derive the projected rotational velocity, \textit{v}sin\textit{i}, of the stars belonging to the eMSTO region of the main sequence (MS) utilizing \textit{Gaia}-ESO spectra. Our results reveal a positive correlation between \textit{v}sin\textit{i} and the color of eMSTO stars, where fast-rotating stars predominantly occupy the red part of the MS while slow-rotating ones prefer a bluer side of the MS. The gravity-darkening effect might be a reason for this correlation. We find that most of the close binaries present in the eMSTO population would be slow-rotating due to the tidal-locking phenomenon. We identify four double-lined spectroscopic binaries (SB2) featuring slow-rotating companions, further supporting this tidal-locking hypothesis. However, the spatial distribution and the cumulative radial distribution indicate a higher concentration of red eMSTO stars in the cluster's central region than their bluer counterparts. This suggests that tidal locking is less likely to be the cause of the observed spread in rotation rates among eMSTO stars. Instead, we propose that star-disk interactions during the pre-main-sequence phase might have played a crucial role in spreading the rotation rates of stars, leading to the eMSTO phenomenon in NGC\,6067.

Figures

Figures reproduced from arXiv: 2507.14433 by the authors.

Figure 1
Figure 1. The cluster over-density in the proper motions space. The red points represent potential cluster member stars. Blue points denote the field stars. structed from the identified member stars to estimate the cluster’s age. We took the extinction value to be AV = 0.99 mag as provided by Hunt & Reffert (2023). The best fit was obtained for an isochrone correspond￾ing to a log(age) of 7.96 years, which corresponds to a cl… view at source ↗
Figure 2
Figure 2. The color-magnitude diagram of the cluster NGC 6067. The stars belonging to the eMSTO are shown by black points. The eMSTO stars also include Be stars enclosed by red squares and SB2 stars enclosed by blue squares. The RGB, BSS, and lMS stars are also shown by the markers given in the legend of the figure. The black continuous curve shows the best-fit Marigo et al. (2017) isochrone corresponding to the logarithmic a… view at source ↗
Figure 3
Figure 3. 2D color-map of extinction for the eMSTO stars in NGC 6067 color-coded by AV values taken from Khalatyan et al. (2024). We estimated the radial velocity (RV) and the pro￾jected rotational velocity, vsini, of the stars using spec￾tra from the Gaia-ESO archives. The iSpec software package was used to derive these velocities (Blanco- [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figures from the paper (12 more)
Figure 4
Figure 4. Figure 4: Left panel: observed color-magnitude diagram of NGC 6067 where the reddening vector is shown by an arrow. Middle panel: CMD in the rotated frame which is considered as a new reference frame for the differential reddening measurements. The red curve represent the fiduci…
Figure 5
Figure 5. Figure 5: The comparison between original CMD (left panel) and differential reddening corrected CMD (right panel) of NGC 6067 cluster. Cuaresma et al. 2014; Blanco-Cuaresma 2019). We used the atomic lines from the Vienna Atomic Line Database (VALD) provided by Kupka et al. (1999…
Figure 6
Figure 6. Figure 6: The observed (blue lines) spectrum and best-fit synthetic spectral lines (red lines) for the star with ID 269. The synthetic spectrum was fitted only in segments of 0.1 nm surrounding the selected lines (yellow lines) labeled by corresponding element names on the top o…
Figure 7
Figure 7. Figure 7: The normalized spectra of the Be stars with IDs 355 and 626 are shown in the upper and lower panels, respectively. The emission features are conspicuous in the Hγ (486.1 nm) absorption line of these Be stars. Hβ line in the Be stars indicates them to belong to the shel…
Figure 8
Figure 8. Figure 8: The cross-correlation function of SB2 stars with IDs 70, 609, 643, and 691 found in the eMSTO population of NGC 6067 are shown from top to bottom order, respectively. spectra by minimization of the χ 2 , which is achieved through the MINUIT optimization package provide…
Figure 9
Figure 9. Figure 9: The spectra of the SB2 stars with IDs 70, 609, 643, and 691 are shown by the blue curves (top to bottom), illustrating the best-fit synthetic spectra expressed by yellow curves. The synthetic spectrum fitting for these binary stars is performed by the GIRFIT code [PIT…
Figure 10
Figure 10. Figure 10: The color-magnitude diagram of NGC 6067 color-coded by the projected rotational velocity of the stars. The black rectangle encloses the eMSTO stars of NGC 6067. The green continuous curve represents the fiducial line for the main sequence stars. could be due to gravit…
Figure 11
Figure 11. Figure 11: The correlation between pseudo-color ∆GBP−GRP and vsini for the eMSTO stars. The red points show the outliers. 0.25 0.50 0.75 1.00 1.25 1.50 1.75 2.00 GBP GRP (mag) 8 10 12 14 16 18 G (mag) bMS rMS lMS RGB BSS [PITH_FULL_IMAGE:figures/full_fig_p014_11.png]
Figure 12
Figure 12. Figure 12: Plot exhibiting fiducial line (shown by the black line) and subgroups of stars in the color-magnitude diagram of NGC 6067. The black asterisks represent outlier stars, as identified in [PITH_FULL_IMAGE:figures/full_fig_p014_12.png]
Figure 13
Figure 13. Figure 13: The plot for correlation between mass ratio, separation, and synchronization time for the binaries to be found in the eMSTO population of the cluster NGC 6067. The colormap represents the synchronization time on a logarithmic scale. The red curve indicates the maximum…
Figure 14
Figure 14. Figure 14: Spatial distributions of the bMS and rMS stars in the form of density contours in NGC 6067. A black cross symbol marks the cluster center in the spatial distribution. below: TE = 8.9 × 105 (Nr3 h /m¯ ) 1/2 log(0.4N) where N denotes the total number of member stars. rh…
Figure 15
Figure 15. Figure 15: Cumulative radial distributions of the bMS and rMS stars in NGC 6067. obtained the MSR to be 1.2±0.1 for NGC 6067. The MSR value very close to unity suggest a weak mass seg￾regation in the cluster. Such a weak mass segregation may be due to the fact that the dynamical…

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Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Examining the stellar-merger origin of the blue main sequence in the open cluster NGC\,3532 with N-body simulations

    astro-ph.GA 2026-07 conditional novelty 6.0 of 10

    N-body models of NGC 3532 produce only 0-8 stellar mergers, too few to explain the cluster's ~37% blue main-sequence population, disfavoring the merger origin for its slow rotators.

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Works this paper leans on

69 extracted references · 17 canonical work pages · cited by 1 Pith paper

  1. [1]

    J., Goodwin, S

    Allison, R. J., Goodwin, S. P., Parker, R. J., et al. 2009, mnras, 395, 1449, doi: 10.1111/j.1365-2966.2009.14508.x

    work page arXiv 2009

  2. [2]

    2017, MNRAS, 469, 1330, doi: 10.1093/mnras/stx783

    Alonso-Santiago, J., Negueruela, I., Marco, A., et al. 2017, MNRAS, 469, 1330, doi: 10.1093/mnras/stx783

    work page doi:10.1093/mnras/stx783 2017

  3. [3]

    2021, A&A, 656, A149, doi: 10.1051/0004-6361/202141747

    Alonso-Santiago, J., Frasca, A., Catanzaro, G., et al. 2021, A&A, 656, A149, doi: 10.1051/0004-6361/202141747

    work page doi:10.1051/0004-6361/202141747 2021

  4. [4]

    Amard, L., & Matt, S. P. 2020, ApJ, 889, 108, doi: 10.3847/1538-4357/ab6173

    doi:10.3847/1538-4357/ab6173 2020

  5. [5]

    Amard, L., Roquette, J., & Matt, S. P. 2020, MNRAS, 499, 3481, doi: 10.1093/mnras/staa3038

    work page doi:10.1093/mnras/staa3038 2020

  6. [6]

    Bastian, N., & de Mink, S. E. 2009, MNRAS, 398, L11, doi: 10.1111/j.1745-3933.2009.00696.x

    arXiv 2009

  7. [7]

    2020, MNRAS, 495, 1978, doi: 10.1093/mnras/staa1332

    Bastian, N., Kamann, S., Amard, L., et al. 2020, MNRAS, 495, 1978, doi: 10.1093/mnras/staa1332

    doi:10.1093/mnras/staa1332 2020

  8. [8]

    2018, MNRAS, 480, 3739, doi: 10.1093/mnras/sty2100

    Bastian, N., Kamann, S., Cabrera-Ziri, I., et al. 2018, MNRAS, 480, 3739, doi: 10.1093/mnras/sty2100

    doi:10.1093/mnras/sty2100 2018

Show all 69 references
  1. [9]

    Bekki, K., & Mackey, A. D. 2009, MNRAS, 394, 124, doi: 10.1111/j.1365-2966.2008.14320.x

    2009

  2. [10]

    2019, MNRAS, 486, 2075, doi: 10.1093/mnras/stz549

    Blanco-Cuaresma, S. 2019, MNRAS, 486, 2075, doi: 10.1093/mnras/stz549

    2019 doi

  3. [11]

    2014, A&A, 569, A111, doi: 10.1051/0004-6361/201423945

    Blanco-Cuaresma, S., Soubiran, C., Heiter, U., & Jofr´ e, P. 2014, A&A, 569, A111, doi: 10.1051/0004-6361/201423945

    2014 doi

  4. [12]

    P., Mohanty, S., et al

    Bouvier, J., Matt, S. P., Mohanty, S., et al. 2014, in Protostars and Planets VI, ed. H. Beuther, R. S. Klessen, C. P. Dullemond, & T. Henning, 433–450, doi: 10.2458/azu uapress 9780816531240-ch019

    2014 doi

  5. [13]

    2016, MNRAS, 457, 809, doi: 10.1093/mnras/stv2977

    Cabrera-Ziri, I., Bastian, N., Hilker, M., et al. 2016, MNRAS, 457, 809, doi: 10.1093/mnras/stv2977

    2016 doi

  6. [14]

    2020, A&A, 640, A1, doi: 10.1051/0004-6361/202038192

    Cantat-Gaudin, T., Anders, F., Castro-Ginard, A., et al. 2020, A&A, 640, A1, doi: 10.1051/0004-6361/202038192

    2020 doi

  7. [15]

    A., Clayton, G

    Cardelli, J. A., Clayton, G. C., & Mathis, J. S. 1989, ApJ, 345, 245, doi: 10.1086/167900

    1989 doi

  8. [16]

    Castelli, F., & Kurucz, R. L. 2003, in IAU Symposium, Vol. 210, Modelling of Stellar Atmospheres, ed. N. Piskunov, W. W. Weiss, & D. F. Gray, A20, doi: 10.48550/arXiv.astro-ph/0405087

    2003 doi arXiv

  9. [17]

    2022, MNRAS, 512, 3992, doi: 10.1093/mnras/stab3589

    Chen, J., Li, Z., Zhang, S., Deng, Y., & Zhao, W. 2022, MNRAS, 512, 3992, doi: 10.1093/mnras/stab3589

    2022 doi

  10. [18]

    P., Marino, A

    Cordoni, G., Milone, A. P., Marino, A. F., et al. 2023, A&A, 672, A29, doi: 10.1051/0004-6361/202245457 D’Antona, F., Di Criscienzo, M., Decressin, T., et al. 2015, MNRAS, 453, 2637, doi: 10.1093/mnras/stv1794 D’Antona, F., Dell’Agli, F., Tailo, M., et al. 2023, MNRAS, 521, 44...

    2023 doi

  11. [19]

    2021, A&A, 649, A5, doi: 10.1051/0004-6361/202039834

    Fabricius, C., Luri, X., Arenou, F., et al. 2021, A&A, 649, A5, doi: 10.1051/0004-6361/202039834

    2021 doi

  12. [20]

    R., Mucciarelli, A., Lanzoni, B., et al

    Ferraro, F. R., Mucciarelli, A., Lanzoni, B., et al. 2023, Nature Communications, 14, 2584, doi: 10.1038/s41467-023-38153-w Fr´ emat, Y., Neiner, C., Hubert, A. M., et al. 2006, A&A, 451, 1053, doi: 10.1051/0004-6361:20053305 Gaia Collaboration, Prusti, T., de Bruijne, J. H. J...

    2023 doi

  13. [21]

    2019, A&A, 622, A66, doi: 10.1051/0004-6361/201834505

    Georgy, C., Charbonnel, C., Amard, L., et al. 2019, A&A, 622, A66, doi: 10.1051/0004-6361/201834505

    2019 doi

  14. [22]

    2014, ApJ, 797, 35, doi: 10.1088/0004-637X/797/1/35

    Goudfrooij, P., Girardi, L., Kozhurina-Platais, V., et al. 2014, ApJ, 797, 35, doi: 10.1088/0004-637X/797/1/35

    2014 doi

  15. [23]

    O., & Corbally, C

    Gray, R. O., & Corbally, C. J. 1994, AJ, 107, 742, doi: 10.1086/116893

    1994 doi

  16. [24]

    Grevesse, N., Asplund, M., & Sauval, A. J. 2007, SSRv, 130, 105, doi: 10.1007/s11214-007-9173-7

    2007 doi

  17. [25]

    Groenewegen, M. A. T. 2021, A&A, 654, A20, doi: 10.1051/0004-6361/202140862

    2021 doi

  18. [26]

    G., & Day, C

    Hills, J. G., & Day, C. A. 1976, Astrophys. Lett., 17, 87

    1976

  19. [27]

    1995, ApJ, 439, 875, doi: 10.1086/175226

    Hubeny, I., & Lanz, T. 1995, ApJ, 439, 875, doi: 10.1086/175226

    1995 doi

  20. [28]

    L., & Reffert, S

    Hunt, E. L., & Reffert, S. 2023, A&A, 673, A114, doi: 10.1051/0004-6361/202346285 —. 2024, A&A, 686, A42, doi: 10.1051/0004-6361/202348662

    2023 doi

  21. [29]

    R., Tout, C

    Hurley, J. R., Tout, C. A., & Pols, O. R. 2002, MNRAS, 329, 897, doi: 10.1046/j.1365-8711.2002.05038.x

    2002

  22. [30]

    G., Zanni, C., Matt, S

    Ireland, L. G., Zanni, C., Matt, S. P., & Pantolmos, G. 2021, ApJ, 906, 4, doi: 10.3847/1538-4357/abc828 19

    2021 doi

  23. [31]

    2021, MNRAS, 508, 2302, doi: 10.1093/mnras/stab2643

    Saracino, S. 2021, MNRAS, 508, 2302, doi: 10.1093/mnras/stab2643

    2021 doi

  24. [32]

    2020, MNRAS, 492, 2177, doi: 10.1093/mnras/stz3583

    Kamann, S., Bastian, N., Gossage, S., et al. 2020, MNRAS, 492, 2177, doi: 10.1093/mnras/stz3583

    2020 doi

  25. [33]

    2023, MNRAS, 518, 1505, doi: 10.1093/mnras/stac3170

    Kamann, S., Saracino, S., Bastian, N., et al. 2023, MNRAS, 518, 1505, doi: 10.1093/mnras/stac3170

    2023 doi

  26. [34]

    2024, A&A, 691, A98, doi: 10.1051/0004-6361/202451427

    Khalatyan, A., Anders, F., Chiappini, C., et al. 2024, A&A, 691, A98, doi: 10.1051/0004-6361/202451427

    2024 doi

  27. [35]

    Kraft, R. P. 1967, ApJ, 150, 551, doi: 10.1086/149359

    1967 doi

  28. [36]

    A., Stempels, H

    Kupka, F., Piskunov, N., Ryabchikova, T. A., Stempels, H. C., & Weiss, W. W. 1999, A&AS, 138, 119, doi: 10.1051/aas:1999267

    1999 doi

  29. [37]

    C., & Weiss, W

    Stempels, H. C., & Weiss, W. W. 2000, Baltic Astronomy, 9, 590, doi: 10.1515/astro-2000-0420

    2000 doi

  30. [38]

    Kurucz, R. L. 2005, Memorie della Societa Astronomica Italiana Supplementi, 8, 14

    2005

  31. [39]

    A., Hern´ andez, J., et al

    Lindegren, L., Klioner, S. A., Hern´ andez, J., et al. 2021, A&A, 649, A2, doi: 10.1051/0004-6361/202039709

    2021 doi

  32. [40]

    2017, ApJ, 835, 77, doi: 10.3847/1538-4357/835/1/77

    Marigo, P., Girardi, L., Bressan, A., et al. 2017, ApJ, 835, 77, doi: 10.3847/1538-4357/835/1/77

    2017 doi

  33. [41]

    F., Milone, A

    Marino, A. F., Milone, A. P., Casagrande, L., et al. 2018, ApJL, 863, L33, doi: 10.3847/2041-8213/aad868

    2018 doi

  34. [42]

    Matt, S., & Pudritz, R. E. 2005, ApJL, 632, L135, doi: 10.1086/498066

    2005 doi

  35. [43]

    C., Samal, M

    Maurya, J., Joshi, Y. C., Samal, M. R., Rawat, V., & Gour, A. S. 2023, Journal of Astrophysics and Astronomy, 44, 71, doi: 10.1007/s12036-023-09959-3

    2023 doi

  36. [44]

    R., Amard, L., et al

    Maurya, J., Samal, M. R., Amard, L., et al. 2024, MNRAS, 532, 1212, doi: 10.1093/mnras/stae1611

    2024 doi

  37. [45]

    McCrea, W. H. 1964, MNRAS, 128, 147, doi: 10.1093/mnras/128.2.147

    1964 doi

  38. [46]

    2017, The Journal of Open Source Software, 2, 205, doi: 10.21105/joss.00205

    McInnes, L., Healy, J., & Astels, S. 2017, The Journal of Open Source Software, 2, 205, doi: 10.21105/joss.00205

    2017 doi

  39. [47]

    2017, A&A, 608, A95, doi: 10.1051/0004-6361/201730442

    Merle, T., Van Eck, S., Jorissen, A., et al. 2017, A&A, 608, A95, doi: 10.1051/0004-6361/201730442

    2017 doi

  40. [48]

    P., Bedin, L

    Milone, A. P., Bedin, L. R., Piotto, G., & Anderson, J. 2009, A&A, 497, 755, doi: 10.1051/0004-6361/200810870

    2009 doi

  41. [49]

    P., Piotto, G., Bedin, L

    Milone, A. P., Piotto, G., Bedin, L. R., et al. 2012, A&A, 540, A16, doi: 10.1051/0004-6361/201016384

    2012 doi

  42. [50]

    2011, A&A, 528, A44, doi: 10.1051/0004-6361/201015814

    Mucciarelli, A. 2011, A&A, 528, A44, doi: 10.1051/0004-6361/201015814

    2011 doi

  43. [51]

    2019, The Journal of Open Source Software, 4, 1721, doi: 10.21105/joss.01721

    Naidoo, K. 2019, The Journal of Open Source Software, 4, 1721, doi: 10.21105/joss.01721

    2019 doi

  44. [52]

    2024, A&A, 689, A162, doi: 10.1051/0004-6361/202450255

    Niederhofer, F., Bellini, A., Kozhurina-Platais, V., et al. 2024, A&A, 689, A162, doi: 10.1051/0004-6361/202450255

    2024 doi

  45. [53]

    C., Mathieu, R

    Nine, A. C., Mathieu, R. D., Schuler, S. C., & Milliman, K. E. 2024, ApJ, 970, 187, doi: 10.3847/1538-4357/ad534b

    2024 doi

  46. [54]

    2003, A&A, 399, 603, doi: 10.1051/0004-6361:20021759

    Palacios, A., Talon, S., Charbonnel, C., & Forestini, M. 2003, A&A, 399, 603, doi: 10.1051/0004-6361:20021759

    2003 doi

  47. [55]

    M., & Rivinius, T

    Porter, J. M., & Rivinius, T. 2003, PASP, 115, 1153, doi: 10.1086/378307

    2003 doi

  48. [56]

    2022, A&A, 666, A121, doi: 10.1051/0004-6361/202243141

    Randich, S., Gilmore, G., Magrini, L., et al. 2022, A&A, 666, A121, doi: 10.1051/0004-6361/202243141

    2022 doi

  49. [57]

    E., Frinchaboy, P

    Ray, A. E., Frinchaboy, P. M., Donor, J., Chojnowski, S. D., & Melendez, M. 2022, AJ, 163, 195, doi: 10.3847/1538-3881/ac5835

    2022 doi

  50. [58]

    Reddy, A. B. S., Giridhar, S., & Lambert, D. L. 2013, MNRAS, 431, 3338, doi: 10.1093/mnras/stt412

    2013 doi

  51. [59]

    W., et al

    Riello, M., De Angeli, F., Evans, D. W., et al. 2021, A&A, 649, A3, doi: 10.1051/0004-6361/202039587

    2021 doi

  52. [60]

    C., & Martayan, C

    Rivinius, T., Carciofi, A. C., & Martayan, C. 2013, A&A Rv, 21, 69, doi: 10.1007/s00159-013-0069-0

    2013 doi

  53. [61]

    2006, A&A, 459, 137, doi: 10.1051/0004-6361:20053008

    Rivinius, T., ˇStefl, S., & Baade, D. 2006, A&A, 459, 137, doi: 10.1051/0004-6361:20053008

    2006 doi

  54. [62]

    2021, MNRAS, 508, 3710, doi: 10.1093/mnras/stab2772

    Stasevic, S. 2021, MNRAS, 508, 3710, doi: 10.1093/mnras/stab2772

    2021 doi

  55. [63]

    Sills, A., & Pinsonneault, M. H. 2000, ApJ, 540, 489, doi: 10.1086/309306

    2000 doi

  56. [64]

    Spitzer, Lyman, J., & Hart, M. H. 1971, ApJ, 164, 399, doi: 10.1086/150855

    1971 doi

  57. [65]

    Sun, W., de Grijs, R., Deng, L., & Albrow, M. D. 2021, MNRAS, 502, 4350, doi: 10.1093/mnras/stab347

    2021 doi

  58. [66]

    2019, ApJ, 883, 182, doi: 10.3847/1538-4357/ab3cd0

    Sun, W., Li, C., Deng, L., & de Grijs, R. 2019, ApJ, 883, 182, doi: 10.3847/1538-4357/ab3cd0

    2019 doi

  59. [67]

    Turner, D. G. 2016, RMxAA, 52, 223, doi: 10.48550/arXiv.1603.02276

    2016 doi arXiv

  60. [68]

    M., Beccari, G., et al

    Venuti, L., Cody, A. M., Beccari, G., et al. 2024, AJ, 167, 120, doi: 10.3847/1538-3881/ad1f65 von Zeipel, H. 1924, MNRAS, 84, 665, doi: 10.1093/mnras/84.9.665

    2024 doi

  61. [69]

    2022, Nature Astronomy, 6, 480, doi: 10.1038/s41550-021-01597-5

    Wang, C., Langer, N., Schootemeijer, A., et al. 2022, Nature Astronomy, 6, 480, doi: 10.1038/s41550-021-01597-5

    2022 doi

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