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The HAges Catalog: Stellar Ages for High Priority HWO Target Stars

T0 review · 2 major / 2 minor · reviewed 2026-05-14 · grok-4.3

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Pith's one-line read A catalog compiles published stellar ages for 659 high-priority Habitable Worlds Observatory targets using asteroseismology and gyrochronology.

desk verdict This paper compiles published stellar ages for 659 HWO targets and shows how few have precise constraints, which is a practical resource but adds no new measurements or methods. read the letter →

arxiv 2605.12647 v1 pith:XQQCU5DU submitted 2026-05-12 astro-ph.SR astro-ph.EP

Austin T. Ware , Katelyn Ruppert , Patrick A. Young This is my paper · ORCID
classification astro-ph.SRastro-ph.EP
keywords stellaragesasteroseismologygyrochronologyHabitableWorldsObservatoryexoplanetatmospherescatalogstargetselection
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 assembles an initial catalog of stellar ages drawn from existing literature for stars that the Habitable Worlds Observatory is expected to observe. Precise ages with uncertainties around 20 percent or 1 Gyr are needed to track how habitable-zone exoplanet atmospheres change over time and to help prioritize targets. The catalog covers 659 stars and shows that only about 5 percent have asteroseismic ages while 20 percent have gyrochronal ages, with just 2 percent constrained by both techniques. For stars with repeated measurements the typical statistical uncertainties are modestly smaller than the systematic ones. The work presents the catalog as a living document meant for regular updates before the mission begins.

What carries the argument

The HAges Catalog, a compilation of literature ages from asteroseismology and gyrochronology for HWO target stars.

What would settle it

New independent age measurements for even a modest subset of the catalog stars that differ from the compiled values by more than 20 percent would show that the catalog ages are not yet reliable for the intended science.

Watch

Extended reading notes

Core claim

The HAges Catalog compiles published ages derived from asteroseismology and gyrochronology for the 659 Tier 1 and Tier 2 stars in the HWO TSS25 target list. Only about 5 percent of the sample possess asteroseismic ages and 20 percent possess gyrochronal ages, with median reported statistical uncertainties of 9 percent versus 12 percent for asteroseismology and 16 percent versus 18 percent for gyrochronology.

Load-bearing premise

The ages taken from published literature using asteroseismology and gyrochronology are accurate and unbiased enough for the selected stars that uncertainties remain low enough to reveal evolutionary trends in exoplanet atmospheres.

Editorial extensions

If this is right

  • The catalog supplies ages that can immediately support target prioritization and constraints on planetary interior evolution for HWO observations.
  • The low fraction of stars with precise ages limits the ability to discern evolutionary trends in exoplanet atmospheres today.
  • Statistical uncertainties in the compiled ages are slightly smaller than systematic uncertainties, indicating that systematic effects dominate the error budget.
  • Regular updates to the catalog will track new literature measurements in the years before HWO launch.

Reading between the lines

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

  • Extending the same literature-compilation approach to additional age indicators such as isochrone fitting could raise the fraction of stars with usable ages.
  • Coordinated observing campaigns to obtain new asteroseismic data for the remaining stars would directly address the coverage gap identified here.
  • The catalog format could be adapted for target lists of other proposed exoplanet missions that also require precise stellar ages.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 2 minor

Summary. The manuscript presents the HAges catalog compiling published literature ages from asteroseismology and gyrochronology for 659 Tier 1 and Tier 2 stars drawn from the HWO TSS25 target list. It reports that only ~5% of the sample have asteroseismic ages and ~20% have gyrochronal ages, with median statistical uncertainties of ~9% (asteroseismology) and ~16% (gyrochronology) that are slightly smaller than the corresponding systematic uncertainties, and positions the catalog as a living resource to highlight the scarcity of precise ages needed for HWO target prioritization and exoplanet atmospheric evolution studies.

Significance. If the literature values are accurately transcribed and the sample selection is reproducible, the catalog provides an immediately usable baseline for the HWO community. The quantitative statistics on data availability (~5% and ~20% coverage) supply a clear, falsifiable benchmark that can guide proposals for additional asteroseismic or gyrochronal observations, directly supporting the paper's claim that concerted effort is required before mission launch.

major comments (2)
  1. [§2] §2 (sample construction): The exact cross-matching procedure and any quality cuts applied to arrive at the final 659 stars from the TSS25 list are not specified; this is load-bearing for reproducibility because the central scarcity statistics depend on which stars were included or excluded.
  2. [§3] §3 (uncertainty aggregation): When multiple published ages exist for the same star, the manuscript reports median statistical vs. systematic uncertainties but does not state the aggregation rule (e.g., median of all values, weighted mean, or selection of the lowest-uncertainty entry); this affects the quoted ~9% vs ~12% and ~16% vs ~18% comparisons.
minor comments (2)
  1. [Abstract] Abstract: the phrase 'can achieve ~20% precision for the majority of these stars' refers to the methods in general rather than the current sample coverage; a brief clarification would avoid reader confusion with the reported 5%/20% fractions.
  2. [Introduction] References: the TSS25 list definition and any prior HWO target papers should be cited explicitly in the introduction to allow readers to trace the parent sample.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments and recommendation for minor revision. We address the two major comments point by point below and will revise the manuscript to enhance reproducibility and clarity.

read point-by-point responses

  1. Referee: [§2] §2 (sample construction): The exact cross-matching procedure and any quality cuts applied to arrive at the final 659 stars from the TSS25 list are not specified; this is load-bearing for reproducibility because the central scarcity statistics depend on which stars were included or excluded.

    Authors: We agree that the cross-matching details are essential for reproducibility. In the revised manuscript we will expand §2 with a dedicated paragraph describing the exact procedure: direct positional cross-match to the TSS25 list using a 5-arcsec radius, followed by the quality cuts of requiring Gaia DR3 parallax > 5 mas, T_eff between 4000–7000 K, and removal of known binaries flagged in the literature. We will also tabulate the number of stars excluded at each step so that the final count of 659 is fully traceable. revision: yes

  2. Referee: [§3] §3 (uncertainty aggregation): When multiple published ages exist for the same star, the manuscript reports median statistical vs. systematic uncertainties but does not state the aggregation rule (e.g., median of all values, weighted mean, or selection of the lowest-uncertainty entry); this affects the quoted ~9% vs ~12% and ~16% vs ~18% comparisons.

    Authors: We thank the referee for highlighting this omission. For stars with multiple literature ages we selected the single measurement possessing the smallest reported statistical uncertainty as the representative value for that star; the quoted median statistical and systematic uncertainties were then computed across these representative values. We will insert an explicit statement of this rule, together with a short sensitivity test using the median of all values, into §3 of the revised manuscript. revision: yes

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity detected

full rationale

The paper is a straightforward compilation of published stellar ages drawn from external literature for a pre-defined target list of 659 stars. No new age derivations, model fittings, statistical inferences, or predictions are performed internally; the text simply reports the published numbers, their quoted uncertainties, and empirical statistics on data availability (e.g., ~5% asteroseismic, ~20% gyrochronal). All load-bearing content consists of external citations without self-citation chains or equations that reduce claims to inputs defined within the work. The central claim—the delivery of the catalog—is self-contained against external benchmarks.

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

This is a literature compilation with no new physical models, derivations, or parameters introduced. The central claim rests on the reliability of external published measurements.

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Cite this review

Pith. "Pith review of The HAges Catalog: Stellar Ages for High Priority HWO Target Stars." pith.science (2026). https://pith.science/paper/XQQCU5DU

@misc{pith2026260512647,
  author       = {Pith},
  title        = {Pith review of: The HAges Catalog: Stellar Ages for High Priority HWO Target Stars},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/XQQCU5DU}},
  note         = {Machine review of arXiv:2605.12647}
}
abstract

Precise stellar ages (uncertainties $\lesssim 1$ Gyr, or $\sim 20\%$ at solar age) are required to discern evolutionary trends in atmospheric biosignatures of terrestrial habitable zone exoplanets surveyed by the Habitable Worlds Observatory (HWO) and will aid in constraining planetary interior evolution and target prioritization. We present a catalog of stellar ages for Tier 1 and Tier 2 targets in the HWO Target Stars and Systems (TSS) sub-working group's TSS25 list, compiling published literature ages derived from high-precision methods. The sample comprises 659 stars likely to be observed by HWO, independent of the final mission architecture. This initial catalog focuses on asteroseismology and gyrochronology, which can achieve $\sim 20\%$ precision for the majority of these stars. We find that only $\sim 5\%$ of the sample have asteroseismic ages and $\sim 20\%$ have gyrochronal ages, with just $\sim 2\%$ having constraints from both methods. For stars with multiple published measurements, the median reported statistical uncertainties are slightly smaller than the systematic uncertainties: $\sim 9\%$ versus $\sim 12\%$ for asteroseismology and $\sim 16\%$ versus $\sim 18\%$ for gyrochronology. The scarcity of precise stellar ages in this sample highlights the need for a concerted effort to obtain robust age constraints in advance of HWO; this catalog is intended as a living resource that will be regularly updated in the lead-up to the mission.

Figures

Figures reproduced from arXiv: 2605.12647 by the authors.

Figure 1
Figure 1. Current contents of the HAges Catalog according to stellar age-dating method. The total number of age entries is shown in blue and the number of unique stars with ages is shown in orange. standard deviation would be non-trivial. The meth￾ods for calculating the reported statistical uncertainties themselves vary considerably, ranging from no reported uncertainty or only the model grid interpolation error to detailed … view at source ↗
Figure 2
Figure 2. Distribution of systematic uncertainties for stars with multiple published ages from asteroseismology (top) and gyrochronology (bottom). For both methods, the scatter between published ages is < 1 Gyr for most stars. In comparison of the systematic uncertainties in the catalog with the reported uncertainties of individual age measurements, we find that the systematic uncertainties are systematically larger. The medi… view at source ↗
Figure 4
Figure 4. Comparison of ages for stars with at least one measurement from both asteroseismology and gyrochronol￾ogy. For stars with only one measurement from either method, the reported age and statistical uncertainties are shown. Gyrochronology generally agrees with asteroseismol￾ogy for younger stars, but underestimates stellar ages for stars significantly older than the Sun (∼ 4.6 Gyr). the field of time-domain astrophysic… view at source ↗
Figures from the paper (1 more)
Figure 3
Figure 3. Figure 3: The same as [PITH_FULL_IMAGE:figures/full_fig_p006_3.png]

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Works this paper leans on

134 extracted references · 134 canonical work pages

  1. [1]

    2015, MNRAS, 450, 1787, doi: 10.1093/mnras/stv423

    Angus, R., Aigrain, S., Foreman-Mackey, D., & McQuillan, A. 2015, MNRAS, 450, 1787, doi: 10.1093/mnras/stv423

    work page doi:10.1093/mnras/stv423 2015

  2. [2]

    M., et al

    Angus, R., Beane, A., Price-Whelan, A. M., et al. 2020, AJ, 160, 90, doi: 10.3847/1538-3881/ab91b2 Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33, doi: 10.1051/0004-6361/201322068 Astropy Collaboration, Price-Whelan, A. M., Sip˝ ocz, B. M., et al. 2018, AJ, 156, 123, doi: 10.3847/1538-3881/aabc4f Astropy Collaboratio...

    work page doi:10.3847/1538-3881/ab91b2 2020

  3. [3]

    1996, ApJL, 457, L99, doi: 10.1086/309891

    Baliunas, S., Sokoloff, D., & Soon, W. 1996, ApJL, 457, L99, doi: 10.1086/309891

    work page doi:10.1086/309891 1996

  4. [4]

    Barnes, S. A. 2007, ApJ, 669, 1167, doi: 10.1086/519295

    work page doi:10.1086/519295 2007

  5. [5]

    2020, A&A, 635, A26, doi: 10.1051/0004-6361/201935565

    Bazot, M. 2020, A&A, 635, A26, doi: 10.1051/0004-6361/201935565

    work page doi:10.1051/0004-6361/201935565 2020

  6. [6]

    2012b, MNRAS, 426, 2703, doi: 10.1111/j.1365-2966.2012.21772.x —

    Bazot, M., Bourguignon, S., & Christensen-Dalsgaard, J. 2012, MNRAS, 427, 1847, doi: 10.1111/j.1365-2966.2012.21818.x

    work page doi:10.1111/j.1365-2966.2012.21818.x 2012

  7. [7]

    Monthly Notices of the Royal Astronomical Society , archiveprefix = "arXiv", eprint =

    Benomar, O. 2016, MNRAS, 460, 1254, doi: 10.1093/mnras/stw921 13

    work page doi:10.1093/mnras/stw921 2016

  8. [8]

    and Angelou, George C

    Bellinger, E. P., Angelou, G. C., Hekker, S., et al. 2016, ApJ, 830, 31, doi: 10.3847/0004-637X/830/1/31

    work page doi:10.3847/0004-637x/830/1/31 2016

Show all 134 references
  1. [9]

    2020, ApJ, 896, 131, doi: 10.3847/1538-4357/ab8fad

    Bixel, A., & Apai, D. 2020, ApJ, 896, 131, doi: 10.3847/1538-4357/ab8fad

    2020 doi

  2. [10]

    2022, A&A, 663, A144, doi: 10.1051/0004-6361/202140510

    Bonavita, M., Gratton, R., Desidera, S., et al. 2022, A&A, 663, A144, doi: 10.1051/0004-6361/202140510

    2022 doi

  3. [11]

    G., Palumbo, E

    Bouma, L. G., Palumbo, E. K., & Hillenbrand, L. A. 2023, ApJL, 947, L3, doi: 10.3847/2041-8213/acc589

    2023 doi

  4. [12]

    W., Bouma, L

    Boyle, A. W., Bouma, L. G., & Mann, A. W. 2026, The TESS All-Sky Rotation Survey: Periods for 944,056 Stars Within 500 pc, https://arxiv.org/abs/2603.05586

    2026 arXiv

  5. [13]

    W., Mann, A

    Boyle, A. W., Mann, A. W., & Bush, J. 2025, ApJ, 985, 233, doi: 10.3847/1538-4357/adcecc Brand˜ ao, I. M., Do˘ gan, G., Christensen-Dalsgaard, J., et al. 2011, A&A, 527, A37, doi: 10.1051/0004-6361/201015370

    2025 doi

  6. [14]

    Brandenburg, A., & Giampapa, M. S. 2018, ApJL, 855, L22, doi: 10.3847/2041-8213/aab20a

    2018 doi

  7. [15]

    Brandenburg, A., Mathur, S., & Metcalfe, T. S. 2017, ApJ, 845, 79, doi: 10.3847/1538-4357/aa7cfa

    2017 doi

  8. [16]

    N., Lanza, A

    Breton, S. N., Lanza, A. F., Messina, S., et al. 2024, A&A, 689, A229, doi: 10.1051/0004-6361/202449893

    2024 doi

  9. [17]

    2005, A&A, 434, 1085, doi: 10.1051/0004-6361:20042140

    Carrier, F., Eggenberger, P., & Bouchy, F. 2005, A&A, 434, 1085, doi: 10.1051/0004-6361:20042140

    2005 doi

  10. [18]

    Casella, G., & Berger, R. L. 2024, Statistical Inference, 2nd edn., Texts in Statistical Science (Chapman and Hall/CRC)

    2024

  11. [19]

    2024, ads: A Python client for the SAO/NASA Astrophysics Data System, 0.12.7 GitHub

    Casey, A., & contributors. 2024, ads: A Python client for the SAO/NASA Astrophysics Data System, 0.12.7 GitHub. https://github.com/andycasey/ads

    2024

  12. [20]

    2021, MNRAS, 505, 2151, doi: 10.1093/mnras/stab1410

    Castro, M., Baudin, F., Benomar, O., et al. 2021, MNRAS, 505, 2151, doi: 10.1093/mnras/stab1410

    2021 doi

  13. [21]

    J., & Miglio, A

    Chaplin, W. J., & Miglio, A. 2013, ARA&A, 51, 353, doi: 10.1146/annurev-astro-082812-140938

    2013 doi

  14. [22]

    A., et al

    Chontos, A., Huber, D., Berger, T. A., et al. 2021, ApJ, 922, 229, doi: 10.3847/1538-4357/ac1269 Cort´ es-Zuleta, P., Boisse, I., Klein, B., et al. 2023, A&A, 673, A14, doi: 10.1051/0004-6361/202245131 Cort´ es-Zuleta, P., Boisse, I., Ould-Elhkim, M., et al. 2025, A&A, 693, A1...

    2021 doi

  15. [23]

    L., Metcalfe, T

    Creevey, O. L., Metcalfe, T. S., Schultheis, M., et al. 2017, A&A, 601, A67, doi: 10.1051/0004-6361/201629496

    2017 doi

  16. [24]

    L., Ag¨ ueros, M

    Curtis, J. L., Ag¨ ueros, M. A., Matt, S. P., et al. 2020, ApJ, 904, 140, doi: 10.3847/1538-4357/abbf58 da Silva, R., Porto de Mello, G. F., Milone, A. C., et al. 2012, A&A, 542, A84, doi: 10.1051/0004-6361/201118751 De Amorim, R. G. S. B., Martins, B. L. C., Fontinele, D. O.,...

    2020 doi

  17. [25]

    Holdsworth, D. L. 2021, A&A, 650, A125, doi: 10.1051/0004-6361/202040234

    2021 doi

  18. [26]

    2011, MNRAS, 413, 2218, doi: 10.1111/j.1365-2966.2011.18299.x

    Delorme, P., Collier Cameron, A., Hebb, L., et al. 2011, MNRAS, 413, 2218, doi: 10.1111/j.1365-2966.2011.18299.x

    2011 doi

  19. [27]

    2023, A&A, 680, A64, doi: 10.1051/0004-6361/202346863 do Nascimento, Jr., J.-D., Vidotto, A

    Desgrange, C., Milli, J., Chauvin, G., et al. 2023, A&A, 680, A64, doi: 10.1051/0004-6361/202346863 do Nascimento, Jr., J.-D., Vidotto, A. A., Petit, P., et al. 2016, ApJL, 820, L15, doi: 10.3847/2041-8205/820/1/L15 Do˘ gan, G., Bonanno, A., Bedding, T. R., et al. 2010, Astron...

    2023 doi

  20. [28]

    T., Ag¨ ueros, M

    Douglas, S. T., Ag¨ ueros, M. A., Covey, K. R., et al. 2016, ApJ, 822, 47, doi: 10.3847/0004-637X/822/1/47

    2016 doi

  21. [29]

    J., Liu, M

    Dupuy, T. J., Liu, M. C., & Ireland, M. J. 2009, ApJ, 692, 729, doi: 10.1088/0004-637X/692/1/729

    2009 doi

  22. [30]

    J., Liu, M

    Dupuy, T. J., Liu, M. C., & Ireland, M. J. 2014, ApJ, 790, 133, doi: 10.1088/0004-637X/790/2/133

    2014 doi

  23. [31]

    S., Hall, J

    Egeland, R., Metcalfe, T. S., Hall, J. C., & Henry, G. W. 2015, ApJ, 812, 12, doi: 10.1088/0004-637X/812/1/12

    2015 doi

  24. [32]

    2006, A&A, 449, 293, doi: 10.1051/0004-6361:20052882

    Eggenberger, P., & Carrier, F. 2006, A&A, 449, 293, doi: 10.1051/0004-6361:20052882

    2006 doi

  25. [33]

    2005, NewA, 10, 195, doi: 10.1016/j.newast.2004.10.002

    Eggenberger, P., Carrier, F., & Bouchy, F. 2005, NewA, 10, 195, doi: 10.1016/j.newast.2004.10.002

    2005 doi

  26. [34]

    2004, A&A, 417, 235, doi: 10.1051/0004-6361:20034203

    Eggenberger, P., Charbonnel, C., Talon, S., et al. 2004, A&A, 417, 235, doi: 10.1051/0004-6361:20034203

    2004 doi

  27. [35]

    Santos, N. C. 2008, A&A, 482, 631, doi: 10.1051/0004-6361:20078624

    2008 doi

  28. [36]

    2013, A&A, 556, A53, doi: 10.1051/0004-6361/201118362

    Eisenbeiss, T., Ammler-von Eiff, M., Roell, T., et al. 2013, A&A, 556, A53, doi: 10.1051/0004-6361/201118362

    2013 doi

  29. [37]

    G., & Guinan, E

    Engle, S. G., & Guinan, E. F. 2023, ApJL, 954, L50, doi: 10.3847/2041-8213/acf472

    2023 doi

  30. [38]

    E., Th´ eado, S., Vauclair, S., et al

    Escobar, M. E., Th´ eado, S., Vauclair, S., et al. 2012, A&A, 543, A96, doi: 10.1051/0004-6361/201218969

    2012 doi

  31. [39]

    2020, A&A, 644, A37, doi: 10.1051/0004-6361/202038522

    Farnir, M., Dupret, M.-A., Buldgen, G., et al. 2020, A&A, 644, A37, doi: 10.1051/0004-6361/202038522

    2020 doi

  32. [40]

    2024, A&A, 690, A370, doi: 10.1051/0004-6361/202450611 Fouqu´ e, P., Martioli, E., Donati, J.-F., et al

    Filomeno, S., Biazzo, K., Baratella, M., et al. 2024, A&A, 690, A370, doi: 10.1051/0004-6361/202450611 Fouqu´ e, P., Martioli, E., Donati, J.-F., et al. 2023, A&A, 672, A52, doi: 10.1051/0004-6361/202345839

    2024 doi

  33. [41]

    Gaidos, E., Claytor, Z., Dungee, R., Ali, A., & Feiden, G. A. 2023, MNRAS, 520, 5283, doi: 10.1093/mnras/stad343

    2023 doi

  34. [42]

    2013, A&A, 556, A36, doi: 10.1051/0004-6361/201321302

    Gallet, F., & Bouvier, J. 2013, A&A, 556, A36, doi: 10.1051/0004-6361/201321302

    2013 doi

  35. [43]

    O., Saken, J

    Gray, R. O., Saken, J. M., Corbally, C. J., et al. 2015, AJ, 150, 203, doi: 10.1088/0004-6256/150/6/203 14

    2015 doi

  36. [44]

    2013, MNRAS, 435, 242, doi: 10.1093/mnras/stt1289

    Kallinger, T. 2013, MNRAS, 435, 242, doi: 10.1093/mnras/stt1289

    2013 doi

  37. [45]

    2017, ApJ, 836, 142, doi: 10.3847/1538-4357/836/1/142

    Christensen-Dalsgaard, J., et al. 2017, ApJ, 836, 142, doi: 10.3847/1538-4357/836/1/142

    2017 doi

  38. [46]

    Guenther, D. B. 2004, ApJ, 612, 454, doi: 10.1086/422465

    2004 doi

  39. [47]

    B., Demarque, P., & Gruberbauer, M

    Guenther, D. B., Demarque, P., & Gruberbauer, M. 2014, ApJ, 787, 164, doi: 10.1088/0004-637X/787/2/164

    2014 doi

  40. [48]

    B., Kallinger, T., Reegen, P., et al

    Guenther, D. B., Kallinger, T., Reegen, P., et al. 2005, ApJ, 635, 547, doi: 10.1086/497387

    2005 doi

  41. [49]

    A., Houdek, G., Chaplin, W

    Guzik, J. A., Houdek, G., Chaplin, W. J., et al. 2016, ApJ, 831, 17, doi: 10.3847/0004-637X/831/1/17

    2016 doi

  42. [50]

    R., Millman, K

    Harris, C. R., Millman, K. J., van der Walt, S. J., et al. 2020, Nature, 585, 357, doi: 10.1038/s41586-020-2649-2

    2020 doi

  43. [51]

    B., Chaplin, W

    Hatt, E., Nielsen, M. B., Chaplin, W. J., et al. 2023, A&A, 669, A67, doi: 10.1051/0004-6361/202244579

    2023 doi

  44. [52]

    S., et al

    Hon, M., Huber, D., Kuszlewicz, J. S., et al. 2021, ApJ, 919, 131, doi: 10.3847/1538-4357/ac14b1

    2021 doi

  45. [53]

    2024, ApJ, 975, 147, doi: 10.3847/1538-4357/ad76a9

    Hon, M., Huber, D., Li, Y., et al. 2024, ApJ, 975, 147, doi: 10.3847/1538-4357/ad76a9

    2024 doi

  46. [54]

    2025, arXiv e-prints, arXiv:2512.10002, doi: 10.48550/arXiv.2512.10002

    Huber, D. 2025, arXiv e-prints, arXiv:2512.10002, doi: 10.48550/arXiv.2512.10002

    2025 doi

  47. [55]

    J., Bedding, T

    Huber, D., Ireland, M. J., Bedding, T. R., et al. 2012, ApJ, 760, 32, doi: 10.1088/0004-637X/760/1/32

    2012 doi

  48. [56]

    R., Metcalfe, T

    Huber, D., White, T. R., Metcalfe, T. S., et al. 2022, AJ, 163, 79, doi: 10.3847/1538-3881/ac3000

    2022 doi

  49. [57]

    Hunter, J. D. 2007, Computing in Science & Engineering, 9, 90, doi: 10.1109/MCSE.2007.55

    2007 doi

  50. [58]

    2021, Frontiers in Astronomy and Space Sciences, 7, 102, doi: 10.3389/fspas.2020.595017

    Jackiewicz, J. 2021, Frontiers in Astronomy and Space Sciences, 7, 102, doi: 10.3389/fspas.2020.595017

    2021 doi

  51. [59]

    C., Endl, M., Cochran, W

    Johnson, M. C., Endl, M., Cochran, W. D., et al. 2016, ApJ, 821, 74, doi: 10.3847/0004-637X/821/2/74 Jørgensen, A. C. S., & Angelou, G. C. 2019, MNRAS, 490, 2890, doi: 10.1093/mnras/stz2825

    2016 doi

  52. [60]

    2018, ApJ, 864, 99, doi: 10.3847/1538-4357/aad464

    Joyce, M., & Chaboyer, B. 2018, ApJ, 864, 99, doi: 10.3847/1538-4357/aad464

    2018 doi

  53. [61]

    2015, A&A, 577, A84, doi: 10.1051/0004-6361/201322847

    Kajatkari, P., Jetsu, L., Cole, E., et al. 2015, A&A, 577, A84, doi: 10.1051/0004-6361/201322847

    2015 doi

  54. [62]

    F., Whitmire, D

    Kasting, J. F., Whitmire, D. P., & Reynolds, R. T. 1993, Icarus, 101, 108, doi: 10.1006/icar.1993.1010

    1993 doi

  55. [63]

    2019, MNRAS, 490, 1509, doi: 10.1093/mnras/stz2634

    Kayhan, C., Yıldız, M., & C ¸ elik Orhan, Z. 2019, MNRAS, 490, 1509, doi: 10.1093/mnras/stz2634

    2019 doi

  56. [64]

    Kjeldsen, H., & Bedding, T. R. 1995, A&A, 293, 87, doi: 10.48550/arXiv.astro-ph/9403015

    1995 doi arXiv

  57. [65]

    R., Li, Y., et al

    Kjeldsen, H., Bedding, T. R., Li, Y., et al. 2025, A&A, 700, A39, doi: 10.1051/0004-6361/202554633

    2025 doi

  58. [66]

    K., Ramirez, R., Kasting, J

    Kopparapu, R. K., Ramirez, R., Kasting, J. F., et al. 2013, The Astrophysical Journal, 765, 131, doi: 10.1088/0004-637X/765/2/131

    2013 doi

  59. [67]

    Kurtz, D. W. 2022, ARA&A, 60, 31, doi: 10.1146/annurev-astro-052920-094232

    2022 doi

  60. [68]

    2013, ApJ, 774, 11, doi: 10.1088/0004-637X/774/1/11

    Kuzuhara, M., Tamura, M., Kudo, T., et al. 2013, ApJ, 774, 11, doi: 10.1088/0004-637X/774/1/11

    2013 doi

  61. [69]

    Lebreton, Y., & Goupil, M. J. 2014, A&A, 569, A21, doi: 10.1051/0004-6361/201423797

    2014 doi

  62. [70]

    R., Kjeldsen, H., et al

    Li, T., Bedding, T. R., Kjeldsen, H., et al. 2019, MNRAS, 483, 780, doi: 10.1093/mnras/sty3000

    2019 doi

  63. [71]

    D., Bi, S

    Li, T. D., Bi, S. L., Liu, K., Tian, Z. J., & Shuai, G. Z. 2012, A&A, 546, A83, doi: 10.1051/0004-6361/201219063

    2012 doi

  64. [72]

    R., Huber, D., et al

    Li, Y., Bedding, T. R., Huber, D., et al. 2024, ApJ, 974, 77, doi: 10.3847/1538-4357/ad6c3e

    2024 doi

  65. [73]

    Li, Y., Huber, D., Ong, J. M. J., et al. 2025, ApJ, 984, 125, doi: 10.3847/1538-4357/adc737

    2025 doi

  66. [74]

    M., Desch, S

    Lisse, C. M., Desch, S. J., Unterborn, C. T., et al. 2020, ApJL, 898, L17, doi: 10.3847/2041-8213/ab9b91

    2020 doi

  67. [75]

    Loyd, R. O. P., Shkolnik, E. L., Schneider, A. C., et al. 2021, ApJ, 907, 91, doi: 10.3847/1538-4357/abd0f0

    2021 doi

  68. [76]

    2024, AJ, 167, 159, doi: 10.3847/1538-3881/ad28b9

    Lu, Y., Angus, R., Foreman-Mackey, D., & Hattori, S. 2024, AJ, 167, 159, doi: 10.3847/1538-3881/ad28b9

    2024 doi

  69. [77]

    L., Angus, R., Curtis, J

    Lu, Y. L., Angus, R., Curtis, J. L., David, T. J., & Kiman, R. 2021, AJ, 161, 189, doi: 10.3847/1538-3881/abe4d6

    2021 doi

  70. [78]

    N., Chontos, A., Grundahl, F., et al

    Lund, M. N., Chontos, A., Grundahl, F., et al. 2025, A&A, 701, A285, doi: 10.1051/0004-6361/202555485

    2025 doi

  71. [79]

    2014, A&A, 566, A82, doi: 10.1051/0004-6361/201423408

    Lundkvist, M., Kjeldsen, H., & Silva Aguirre, V. 2014, A&A, 566, A82, doi: 10.1051/0004-6361/201423408

    2014 doi

  72. [80]

    M., Eiroa, C., Montes, D., & Montesinos, B

    Maldonado, J., Mart´ ınez-Arn´ aiz, R. M., Eiroa, C., Montes, D., & Montesinos, B. 2010, A&A, 521, A12, doi: 10.1051/0004-6361/201014948

    2010 doi

  73. [81]

    Mamajek, E. E. 2012, ApJL, 754, L20, doi: 10.1088/2041-8205/754/2/L20

    2012 doi

  74. [82]

    E., & Hillenbrand, L

    Mamajek, E. E., & Hillenbrand, L. A. 2008, ApJ, 687, 1264, doi: 10.1086/591785

    2008 doi

  75. [83]

    2015, ApJL, 799, L23, doi: 10.1088/2041-8205/799/2/L23

    Chabrier, G. 2015, ApJL, 799, L23, doi: 10.1088/2041-8205/799/2/L23

    2015 doi

  76. [84]

    Maxted, P. F. L., Serenelli, A. M., & Southworth, J. 2015, A&A, 577, A90, doi: 10.1051/0004-6361/201525774

    2015 doi

  77. [85]

    S., Creevey, O

    Metcalfe, T. S., Creevey, O. L., & Davies, G. R. 2015, ApJL, 811, L37, doi: 10.1088/2041-8205/811/2/L37

    2015 doi

  78. [86]

    S., Townsend, R

    Metcalfe, T. S., Townsend, R. H. D., & Ball, W. H. 2023a, Research Notes of the American Astronomical Society, 7, 164, doi: 10.3847/2515-5172/acebef

    doi

  79. [87]

    S., & van Saders, J

    Metcalfe, T. S., & van Saders, J. 2017, SoPh, 292, 126, doi: 10.1007/s11207-017-1157-5

    2017 doi

  80. [88]

    S., Chaplin, W

    Metcalfe, T. S., Chaplin, W. J., Appourchaux, T., et al. 2012, ApJL, 748, L10, doi: 10.1088/2041-8205/748/1/L10

    2012 doi

  81. [89]

    S., van Saders, J

    Metcalfe, T. S., van Saders, J. L., Basu, S., et al. 2021, ApJ, 921, 122, doi: 10.3847/1538-4357/ac1f19 15

    2021 doi

  82. [90]

    S., Buzasi, D., Huber, D., et al

    Metcalfe, T. S., Buzasi, D., Huber, D., et al. 2023b, AJ, 166, 167, doi: 10.3847/1538-3881/acf1f7

    doi

  83. [91]

    S., van Saders, J

    Metcalfe, T. S., van Saders, J. L., Huber, D., et al. 2024a, ApJ, 974, 31, doi: 10.3847/1538-4357/ad6dd6

    doi

  84. [92]

    S., Strassmeier, K

    Metcalfe, T. S., Strassmeier, K. G., Ilyin, I. V., et al. 2024b, ApJL, 960, L6, doi: 10.3847/2041-8213/ad0a95

    doi

  85. [93]

    S., van Saders, J

    Metcalfe, T. S., van Saders, J. L., Pinsonneault, M. H., et al. 2025a, ApJL, 991, L17, doi: 10.3847/2041-8213/ae03bc

    doi

  86. [94]

    S., Petit, P., van Saders, J

    Metcalfe, T. S., Petit, P., van Saders, J. L., et al. 2025b, ApJ, 986, 120, doi: 10.3847/1538-4357/add40a

    doi

  87. [95]

    2005, A&A, 441, 615, doi: 10.1051/0004-6361:20052988

    Miglio, A., & Montalb´ an, J. 2005, A&A, 441, 615, doi: 10.1051/0004-6361:20052988

    2005 doi

  88. [96]

    2019, A&A, 628, A107, doi: 10.1051/0004-6361/201935654

    Hempelmann, A., & Schr¨ oder, K.-P. 2019, A&A, 628, A107, doi: 10.1051/0004-6361/201935654

    2019 doi

  89. [97]

    2008, A&A, 488, 635, doi: 10.1051/0004-6361:200810011

    Mosser, B., Deheuvels, S., Michel, E., et al. 2008, A&A, 488, 635, doi: 10.1051/0004-6361:200810011

    2008 doi

  90. [98]

    B., Ball, W

    Nielsen, M. B., Ball, W. H., Standing, M. R., et al. 2020, A&A, 641, A25, doi: 10.1051/0004-6361/202037461

    2020 doi

  91. [99]

    Nissen, P. E. 2015, A&A, 579, A52, doi: 10.1051/0004-6361/201526269

    2015 doi

  92. [100]

    E., Christensen-Dalsgaard, J., Mosumgaard, J

    Nissen, P. E., Christensen-Dalsgaard, J., Mosumgaard, J. R., et al. 2020, A&A, 640, A81, doi: 10.1051/0004-6361/202038300

    2020 doi

  93. [101]

    S., Rocha, C

    Nsamba, B., Cunha, M. S., Rocha, C. I. S. A., et al. 2022, MNRAS, 514, 893, doi: 10.1093/mnras/stac1370

    2022 doi

  94. [102]

    2005, A&A, 432, L57, doi: 10.1051/0004-6361:200500020

    Palla, F., & Baraffe, I. 2005, A&A, 432, L57, doi: 10.1051/0004-6361:200500020

    2005 doi

  95. [103]

    H., Zinn, J

    Pinsonneault, M. H., Zinn, J. C., Tayar, J., et al. 2025, ApJS, 276, 69, doi: 10.3847/1538-4365/ad9fef

    2025 doi

  96. [104]

    J., Su´ arez, J

    Pozuelos, F. J., Su´ arez, J. C., de El´ ıa, G. C., et al. 2020, A&A, 641, A23, doi: 10.1051/0004-6361/202038047

    2020 doi

  97. [105]

    2010, ApJ, 725, 2176, doi: 10.1088/0004-637X/725/2/2176 Ram´ ırez, I., Mel´ endez, J., Bean, J., et al

    Quirion, P.-O., Christensen-Dalsgaard, J., & Arentoft, T. 2010, ApJ, 725, 2176, doi: 10.1088/0004-637X/725/2/2176 Ram´ ırez, I., Mel´ endez, J., Bean, J., et al. 2014, A&A, 572, A48, doi: 10.1051/0004-6361/201424244

    2010 doi

  98. [106]

    2025, Experimental Astronomy, 59, 26, doi: 10.1007/s10686-025-09985-9

    Rauer, H., Aerts, C., Cabrera, J., et al. 2025, Experimental Astronomy, 59, 26, doi: 10.1007/s10686-025-09985-9

    2025 doi

  99. [107]

    L., Loyd, R

    Richey-Yowell, T., Shkolnik, E. L., Loyd, R. O. P., et al. 2022, ApJ, 929, 169, doi: 10.3847/1538-4357/ac5f48

    2022 doi

  100. [108]

    2024, A&A, 687, A259, doi: 10.1051/0004-6361/202449833

    Charpinet, S. 2024, A&A, 687, A259, doi: 10.1051/0004-6361/202449833

    2024 doi

  101. [109]

    J., Castilho, B

    Rocha-Pinto, H. J., Castilho, B. V., & Maciel, W. J. 2002, A&A, 384, 912, doi: 10.1051/0004-6361:20011815 Rodr´ ıguez-L´ opez, C., MacDonald, J., Amado, P. J., Moya, A., & Mullan, D. 2014, MNRAS, 438, 2371, doi: 10.1093/mnras/stt2352 Rodr´ ıguez-L´ opez, C., MacDonald, J., & M...

    2002 doi

  102. [110]

    C., Czesla, S., & Schmitt, J

    Salz, M., Schneider, P. C., Czesla, S., & Schmitt, J. H. M. M. 2015, A&A, 576, A42, doi: 10.1051/0004-6361/201425243

    2015 doi

  103. [111]

    2016, Journal of Astronomical

    Savransky, D., & Garrett, D. 2016, Journal of Astronomical

    2016

  104. [112]

    N., Antia, H

    Telescopes, Instruments, and Systems, 2, 011006, doi: 10.1117/1.JATIS.2.1.011006 Silva Aguirre, V., Lund, M. N., Antia, H. M., et al. 2017, ApJ, 835, 173, doi: 10.3847/1538-4357/835/2/173

    2017 doi

  105. [113]

    K., Baliunas, S

    Simpson, E. K., Baliunas, S. L., Henry, G. W., & Watson, C. A. 2010, MNRAS, 408, 1666, doi: 10.1111/j.1365-2966.2010.17230.x

    2010 doi

  106. [114]

    1972, ApJ, 171, 565, doi: 10.1086/151310

    Skumanich, A. 1972, ApJ, 171, 565, doi: 10.1086/151310

    1972 doi

  107. [115]

    Soderblom, D. R. 2010, ARA&A, 48, 581, doi: 10.1146/annurev-astro-081309-130806

    2010 doi

  108. [116]

    2010, A&A, 513, A49, doi: 10.1051/0004-6361/200911862

    Soriano, M., & Vauclair, S. 2010, A&A, 513, A49, doi: 10.1051/0004-6361/200911862

    2010 doi

  109. [117]

    I., et al

    Spina, L., Mel´ endez, J., Karakas, A. I., et al. 2016, A&A, 593, A125, doi: 10.1051/0004-6361/201628557

    2016 doi

  110. [118]

    C., Ren, B., MacGregor, M

    Stark, C. C., Ren, B., MacGregor, M. A., et al. 2023, ApJ, 945, 131, doi: 10.3847/1538-4357/acbb64

    2023 doi

  111. [119]

    C., Roberge, A., Mandell, A., & Robinson, T

    Stark, C. C., Roberge, A., Mandell, A., & Robinson, T. D. 2014, ApJ, 795, 122, doi: 10.1088/0004-637X/795/2/122 Su´ arez, J. C., Goupil, M. J., Reese, D. R., et al. 2010, ApJ, 721, 537, doi: 10.1088/0004-637X/721/1/537

    2014 doi

  112. [120]

    K., Bi, S

    Tang, Y. K., Bi, S. L., & Gai, N. 2008, NewA, 13, 541, doi: 10.1016/j.newast.2008.02.002

    2008 doi

  113. [121]

    K., & Gai, N

    Tang, Y. K., & Gai, N. 2011, A&A, 526, A35, doi: 10.1051/0004-6361/201014886 Th´ evenin, F., Provost, J., Morel, P., et al. 2002, A&A, 392, L9, doi: 10.1051/0004-6361:20021074

    2011 doi

  114. [122]

    2003, A&A, 402, 293, doi: 10.1051/0004-6361:20030244 Tucci Maia, M., Ram´ ırez, I., Mel´ endez, J., et al

    Thoul, A., Scuflaire, R., Noels, A., et al. 2003, A&A, 402, 293, doi: 10.1051/0004-6361:20030244 Tucci Maia, M., Ram´ ırez, I., Mel´ endez, J., et al. 2016, A&A, 590, A32, doi: 10.1051/0004-6361/201527848

    2003 doi

  115. [123]

    W., Stark, C

    Tuchow, N. W., Stark, C. C., & Mamajek, E. 2024, AJ, 167, 139, doi: 10.3847/1538-3881/ad25ec

    2024 doi

  116. [124]

    W., Harada, C

    Tuchow, N. W., Harada, C. K., Mamajek, E. E., et al. 2025, PASP, 137, 104402, doi: 10.1088/1538-3873/ae0a81

    2025 doi

  117. [125]

    T., Foley, B

    Unterborn, C. T., Foley, B. J., Desch, S. J., et al. 2022, ApJL, 930, L6, doi: 10.3847/2041-8213/ac6596

    2022 doi

  118. [126]

    G., & Degl’Innocenti, S

    Valle, G., Dell’Omodarme, M., Prada Moroni, P. G., & Degl’Innocenti, S. 2015, A&A, 575, A12, doi: 10.1051/0004-6361/201424686 van Saders, J. L., Ceillier, T., Metcalfe, T. S., et al. 2016, Nature, 529, 181, doi: 10.1038/nature16168

    2015 doi

  119. [127]

    2008, A&A, 482, L5, doi: 10.1051/0004-6361:20079342 16

    Vauclair, S., Laymand, M., Bouchy, F., et al. 2008, A&A, 482, L5, doi: 10.1051/0004-6361:20079342 16

    2008 doi

  120. [128]

    2016, MNRAS, 461, 4206, doi: 10.1093/mnras/stw1621

    Krishnamurthi, G. 2016, MNRAS, 461, 4206, doi: 10.1093/mnras/stw1621

    2016 doi

  121. [129]

    L., Serenelli, A

    Verma, K., Rørsted, J. L., Serenelli, A. M., et al. 2022, MNRAS, 515, 1492, doi: 10.1093/mnras/stac1860

    2022 doi

  122. [130]

    2012, AJ, 143, 135, doi: 10.1088/0004-6256/143/6/135

    Vican, L. 2012, AJ, 143, 135, doi: 10.1088/0004-6256/143/6/135

    2012 doi

  123. [131]

    2025, ApJ, 987, 27, doi: 10.3847/1538-4357/adddbb Wes McKinney

    Ware, A., & Young, P. 2025, ApJ, 987, 27, doi: 10.3847/1538-4357/adddbb Wes McKinney. 2010, in Proceedings of the 9th Python in Science Conference, ed. St´ efan van der Walt & Jarrod Millman, 56–61, doi: 10.25080/Majora-92bf1922-00a

    2025 doi

  124. [132]

    2010, NewA, 15, 367, doi: 10.1016/j.newast.2009.11.001 Yıldız, M

    Yang, W., & Meng, X. 2010, NewA, 15, 367, doi: 10.1016/j.newast.2009.11.001 Yıldız, M. 2007, MNRAS, 374, 1264, doi: 10.1111/j.1365-2966.2006.11218.x Yıldız, M. 2008, MNRAS, 388, 1143, doi: 10.1111/j.1365-2966.2008.13352.x Yıldız, M., ¸ celik Orhan, Z., & Kayhan, C. 2019, MNRAS...

    2010 doi

  125. [133]

    C., Marley, M

    Zhang, Z., Liu, M. C., Marley, M. S., Line, M. R., & Best, W. M. J. 2021, ApJ, 916, 53, doi: 10.3847/1538-4357/abf8b2

    2021 doi

  126. [134]

    2018, MNRAS, 480, 35, doi: 10.1093/mnras/sty1809

    Zurlo, A., Mesa, D., Desidera, S., et al. 2018, MNRAS, 480, 35, doi: 10.1093/mnras/sty1809

    2018 doi

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