Pith. sign in

REVIEW 2 major objections 8 minor 137 references

TOI-7169 b: A Hot Jupiter Transiting a Metal-Poor Star

T0 review · 2 major / 8 minor · reviewed 2026-07-13 · grok-4.5

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read A 12-billion-year-old metal-poor star hosts a confirmed, inflated hot Jupiter.

desk verdict Solid discovery of the lowest-metallicity spectroscopically confirmed host of a transiting giant planet; mass is noisy but the headline result holds. read the letter →

arxiv 2603.25787 v2 pith:5L5LIMVC submitted 2026-03-26 astro-ph.EP astro-ph.SR

Joshua D. Simon , Joseph E. Rodriguez , Jhon Yana Galarza , David W. Latham , Victoria DiTomasso , Karen A. Collins , Jack Schulte , Anirudh Chiti
show 33 more authors
Samuel N. Quinn Mohammad K. Mardini Shubham Kanodia Johanna K. Teske Peter S. Ferguson Samuel W. Yee T. G. Tan Khalid Alsubai Khalid Barkaoui Zouhair Benkhaldoun Krzysztof Bernacki Jaikrit Bhattacharya Jerome P. de Leon Sarah J. Deveny Mark E. Everett Izuru Fukuda Akihiko Fukui Michael Gillon Arvind F. Gupta Steve B. Howell Emmanuel Jehin Gaia Lacedelli Adam Lark Colin Littlefield Felipe Murgas Norio Narita Enric Palle Hannu Parviainen Adam Popowicz Richard P. Schwarz Avi Shporer Abderahmane Soubkiou Francis P. Wilkin
This is my paper
classification astro-ph.EPastro-ph.SR
keywords hotJupitersmetal-poorstarstransitingexoplanetsTESSplanetaryatmospheresMilkyWaydiskalpha-enhancedplanetoccurrence
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

Most known planets orbit metal-rich stars, so it has been hard to test whether giant planets can form when heavy elements are scarce and how those planets differ. This paper reports TOI-7169 b, a short-period giant planet whose host star has a spectroscopically measured metallicity of [Fe/H] = -0.72 and an age of 12.3 Gyr. TESS and ground-based photometry give a 3.44-day period and a radius of 1.475 Jupiter radii; radial-velocity data give a mass of 0.41 Jupiter masses, so the planet is inflated and low-density. The host is alpha-enhanced yet confined to the thin disk. The system therefore supplies a rare, characterizable example of a giant planet born in a low-metallicity environment that has survived for most of cosmic time, and it is a practical target for atmospheric spectroscopy that can test how bulk metallicity shapes giant-planet properties.

What carries the argument

Joint EXOFASTv2 modeling of TESS and multi-band ground photometry with TRES radial velocities, using Gaussian priors on spectroscopically determined stellar mass, radius, temperature, metallicity and age, which yields the planetary radius, mass, density and orbital elements.

What would settle it

A larger set of higher-precision radial velocities that revise the semi-amplitude (and thus mass and density) outside the reported 0.41 +/- 0.14 M_Jup interval, or a higher-resolution spectrum that revises the host [Fe/H] above -0.5, would remove the claim that this is the most metal-poor host of a confirmed inflated transiting giant.

Watch

Extended reading notes

Core claim

TOI-7169 is the most metal-poor ([Fe/H] = -0.72 +/- 0.05) and among the oldest (12.3 +/- 0.6 Gyr) stars currently known to host a confirmed transiting giant planet. The planet has period 3.4373125 d, radius 1.475 +/- 0.029 R_Jup, mass 0.41 +/- 0.14 M_Jup and density ~0.16 g cm^-3; the host is alpha-enhanced but remains on a thin-disk orbit.

Load-bearing premise

The planet mass, and therefore its claimed low density, rests on a radial-velocity semi-amplitude of only 60 +/- 20 m/s measured from nineteen modest-signal spectra.

Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 8 minor

Summary. The manuscript reports the discovery and characterization of TOI-7169 b, a short-period giant planet (P = 3.4373125 d, Rp = 1.475 ± 0.029 R_Jup, Mp = 0.41 ± 0.14 M_Jup) transiting a spectroscopically confirmed metal-poor host ([Fe/H] = −0.72 ± 0.05). The host is further characterized as ancient (12.3 ± 0.6 Gyr), α-enhanced ([α/Fe] ≈ 0.3), and on a thin-disk-like Galactic orbit. Transit confirmation rests on multi-sector TESS photometry plus multi-band ground-based light curves (MuSCAT2, LCOGT, Hamilton), with achromatic depths and high-resolution speckle imaging used to exclude nearby false positives. Stellar parameters come from two independent spectroscopic analyses (uberMS and equivalent-width/MOOG), and planetary parameters from a joint EXOFASTv2 fit of photometry and TRES RVs. The authors argue that TOI-7169 is among the oldest and most metal-poor known hosts of a confirmed transiting giant planet and a promising JWST transmission target (TSM ≈ 93).

Significance. If the host metallicity, age, and transit confirmation hold—as the multi-method evidence indicates—this is a valuable addition to the sparse sample of giant planets around metal-poor stars. Confirmed transiting giants with [Fe/H] ≲ −0.6 have been essentially limited to WASP-98 b and WASP-112 b; a spectroscopically secure host at [Fe/H] = −0.72 with a well-measured radius and multi-band transit validation is therefore of clear interest for occurrence-rate studies, formation metallicity limits, and comparative atmospheric work. Strengths include independent spectroscopic pipelines that agree on [Fe/H], achromatic multi-band transit depths, dual-facility speckle non-detections, a long RV baseline that rules out massive close companions, and a full abundance pattern plus Galactic orbit. The large fractional mass uncertainty is a real limitation on density and inflation claims but does not erase the discovery or the host characterization that drive the paper’s impact.

major comments (2)
  1. §4.2 and Table 6: The planetary mass rests on K = 60 ± 20 m s−1 from 19 modest-S/N TRES spectra (Mp = 0.41 ± 0.14 M_Jup). That fractional uncertainty (~34%) is correctly reported, but the abstract and §5.2 treat the low density (0.159 +0.055/−0.054 g cm−3) and “inflated” status as established facts that then motivate a metallicity–density discussion. Even with the present errors the density is still sub-Jovian at ~1–2σ, so the qualitative claim is not wrong; however, the load-bearing mass/density numbers should be framed more carefully as marginally constrained, and §5.2’s suggestion of a metallicity–density link should be further de-emphasized given that the paper’s own K–S test (Fig. 7) finds no significant difference. Either additional RVs or explicit language that density is secondary and mass-limited would strengthen the central presentation.
  2. §4.1 / Table 4 and abstract: The age 12.3 ± 0.6 Gyr is a Bayesian isochrone posterior with very small statistical errors driven by the precise Gaia parallax and G magnitude. The text notes ~1 Gyr model dependence for old stars and consistency with Dartmouth isochrones and a chemical clock (14.6 ± 3.4 Gyr), which is good, but the abstract and conclusions still quote 12.3 ± 0.6 Gyr without the systematic floor. Because “oldest known” is part of the headline claim, the reported age uncertainty (or at least a clear caveat on absolute isochrone systematics) should be carried into the abstract and §6 so the ranking claim is not overstated relative to other old planet hosts.
minor comments (8)
  1. §3.2: Typo “sourece” → “source” in the MuSCAT2 paragraph.
  2. Table 2 header appears corrupted (“T T Depth”); clarify column names (epoch, mid-transit time, depth) for readability.
  3. Fig. 6 caption/note: The two 2016 RVs are omitted from the time-series panel for visibility; state their consistency with the model explicitly in the caption or text so readers are not left wondering about the long baseline.
  4. §5.2 / Fig. 7: Report the K–S test statistic and p-value (or equivalent) rather than only the qualitative statement that densities are consistent with a single parent distribution.
  5. §5.1: The occurrence-rate back-of-envelope (Boley et al. 2021 upper limit → up to ~100 similar planets among Gaia metal-poor stars) is useful but sensitive to completeness and the applicability of the limit to TESS giants; a sentence on selection biases would help.
  6. §5.3: The thin-disk vs thick-disk discussion is interesting (z_max ~ 200 pc vs thick-disk-like U,V). Consider quoting the Bensby TD/D probability ratio (0.11) earlier when the “thin disk” claim is first made in the abstract/intro for consistency.
  7. Table 5 / Fig. 5: Oxygen is noted as lower than the GALAH trend; a brief comment on whether the NLTE O I 777 nm treatment or continuum placement could drive that offset would help non-specialists.
  8. Throughout: Standardize [α/Fe] notation (≈0.3 in abstract vs 0.29 ± 0.04 from EW analysis) and ensure uberMS vs EW parameters are clearly labeled wherever both appear.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: observational discovery and characterization with independent photometric, spectroscopic, and isochrone constraints.

full rationale

This is a standard exoplanet discovery paper. Stellar metallicity ([Fe/H] = -0.72 ± 0.05) and α-enhancement come from equivalent-width analysis of coadded TRES spectra (ionization/excitation balance with MOOG + Kurucz atmospheres) plus a cross-check with uberMS; age (12.3 ± 0.6 Gyr) and mass follow from Bayesian isochrone fitting (q2 + Yonsei-Yale/Dartmouth) using the spectroscopic parameters, Gaia parallax, and photometry. Planetary period, radius, and mass are obtained from a joint EXOFASTv2 fit to TESS + multi-band ground photometry and TRES RVs, with the spectroscopic stellar parameters imposed only as Gaussian priors. No quantity is fitted to a data subset and then re-presented as a prediction of the same fit; no uniqueness theorem or ansatz is imported via self-citation to force the result; and the headline claim (most metal-poor confirmed transiting giant-planet host) is an empirical ranking against the literature, not a derived identity. Methodological self-citations (EXOFASTv2, uberMS, q2) are ordinary tool references whose outputs are re-derived here from new data and do not close a logical loop.

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

Observational exoplanet discovery paper. Free parameters are the usual fitted orbital and physical quantities; axioms are standard assumptions of transit modeling, LTE abundance analysis, and isochrone fitting. No new physical entities are postulated.

free parameters (4)
  • planetary mass Mp = 0.41 ± 0.14 M_Jup
    Derived from RV semi-amplitude K = 60 ± 20 m s^-1; large uncertainty propagates directly into density.
  • planetary radius Rp = 1.475 ± 0.029 R_Jup
    From transit depth and spectroscopically constrained stellar radius.
  • orbital period P = 3.4373125 d
    Fitted to multi-sector TESS + ground-based transit times.
  • stellar [Fe/H] and age = [Fe/H]=-0.72±0.05, age=12.3±0.6 Gyr
    EW analysis + Yonsei-Yale isochrones with alpha-enhancement correction; adopted as Gaussian priors in EXOFASTv2.
assumptions (4)
  • domain assumption Transit depth equals (Rp/R*)^2 after limb-darkening and dilution corrections; no unaccounted third light.
    Standard transit photometry assumption; supported by multi-band achromatic depths and imaging non-detections (§3.2–3.3).
  • domain assumption LTE radiative transfer and Kurucz ODFNEW atmospheres yield accurate Fe I/II ionization balance for Teff ~ 5700 K, [Fe/H] ~ -0.7.
    Used in q2 EW analysis (§4.1); common for G dwarfs but can carry ~0.05–0.1 dex systematics.
  • domain assumption Yonsei-Yale (and Dartmouth) isochrones with Salaris alpha-correction give reliable ages for old, alpha-enhanced stars.
    Age posterior 12.3 ± 0.6 Gyr (§4.1); absolute ages of old stars remain model-dependent at ~1 Gyr level, as the paper notes.
  • domain assumption RV jitter and circular-orbit prior are adequate; no significant linear trend over 9 yr baseline.
    EXOFASTv2 fit (§4.2); residual jitter 43 m s^-1 is comparable to K.

how reviews work

0 comments
Cite this review

Pith. "Pith review of TOI-7169 b: A Hot Jupiter Transiting a Metal-Poor Star." pith.science (2026). https://pith.science/paper/5L5LIMVC

@misc{pith2026260325787,
  author       = {Pith},
  title        = {Pith review of: TOI-7169 b: A Hot Jupiter Transiting a Metal-Poor Star},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/5L5LIMVC}},
  note         = {Machine review of arXiv:2603.25787}
}
read the original abstract

Most known planets are found around metal-rich host stars, which has made it difficult to determine whether a lower metallicity limit for planet formation exists and how the properties of planets born in low-metallicity environments may differ from those with metal-rich origins. We present the discovery and characterization of TOI-7169 b (TIC 372048733 b), a hot Jupiter that is orbiting a spectroscopically-confirmed metal-poor ([Fe/H] = -0.72 +/- 0.05) host star. Based on photometry from TESS and follow-up ground-based imaging, we measure an orbital period of 3.4373125 d and a planetary radius of 1.475 +/- 0.029 R_Jup. We use TRES spectroscopy to determine a mass for TOI-7169 b of 0.41 +/- 0.14 M_Jup. The planet is therefore inflated, with a low density of 0.159 +0.055/-0.054 g/cm^3. We also characterize the host star, showing that TOI-7169 is ancient (12.3 +/- 0.6 Gyr) and alpha-enhanced ([alpha/Fe] ~ 0.3), but with a Galactocentric orbit that is confined to the thin disk. TOI-7169 is perhaps the oldest and most metal-poor star currently known to host a transiting giant planet. Future transmission spectroscopy probing the atmosphere of TOI-7169 b may provide insight into the effect of metallicity on the physical properties of giant planets.

Figures

Figures reproduced from arXiv: 2603.25787 by the authors.

Figure 1
Figure 1. Flattened TESS light curve of TOI-7169 from Sectors 83 and 84. Sector 83 used an integration time of 120 s and the Sector 84 integration time was 200 s. The 15 transits of TOI-7169 b that occur across these two sectors are indicated by red hash marks. 3. OBSERVATIONS 3.1. TESS TOI-7169 was observed by TESS during its prime mis￾sion and the first two extended missions in Sectors 16, 57, 83, and 84. The TESS observati… view at source ↗
Figure 2
Figure 2. [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Comparison between the spectrum of TOI-7169 (black) and the Sun (blue). The temperatures of the two stars are quite similar, so the differences in line strength are primarily due to abundance differences (with the exception of the very strong Mg line at 5185 ˚A). Spectral lines of iron-peak (Fe and Cr) and α elements (Mg and Ti) are shaded as indicated in the legend. The uberMS fit finds the following parameters for… view at source ↗
Figures from the paper (6 more)
Figure 4
Figure 4. Figure 4: Derived absolute magnitude and effective temper￾ature of TOI-7169 from the q2 package, compared to Yon￾sei-Yale isochrones. The red isochrone represents the best– fitting age, which does not exactly match the derived stellar properties because it is a marginalized Baye…
Figure 5
Figure 5. Figure 5: Abundance pattern of TOI-7169. In each panel, the derived abundance for TOI-7169 is plotted as a red circle, the solar abundance is indicated by the black sun symbol, and abundances of main-sequence stars from GALAH DR4 (S. Buder et al. 2025) are displayed as small gra…
Figure 6
Figure 6. Figure 6: EXOFASTv2 fit results for TOI-7169. The left panel displays the stacked TESS transits and the full transits observed from the ground along with the best-fit model of each. The panel in the upper right plots the TRES radial velocities and the best-fit orbit model, with …
Figure 7
Figure 7. Figure 7: Giant planet densities as a function of host star metallicity. Data are taken from the TEPCat database (J. Southworth 2011). We plot planets with radii between RJ and 1.5 RJ and masses less than 2.0 MJ. TOI-7169 b is displayed as a large red circle. Although it may app…
Figure 8
Figure 8. Figure 8: Galactic orbit of TOI-7169 over the past 1 Gyr. The left panel shows the orbit in the Cartesian x–y plane, the middle panel in the Cartesian x–z plane, and the right panel in cylindrical coordinates. Note the change in y-axis scale between the middle and right panels. …
Figure 9
Figure 9. Figure 9: Toomre diagram for TOI-7169. The dashed curves indicate constant total velocities of 100 km s−1 and 200 km s−1 . Green stars, yellow triangles, and blue squares represent the thin disk (vtot ≤ 60 km s−1 ), tran￾sition/overlap (60 < vtot ≤ 80 km s−1 ), and thick disk (8…

Discussion (0). Sign in to comment.

Reference graph

Works this paper leans on

137 extracted references · 23 canonical work pages

  1. [1]

    W., et al

    Adams Redai, J., Chandra, V., Yee, S. W., et al. 2025, submitted to ApJL, arXiv:2512.06069, doi: 10.48550/arXiv.2512.06069

    work page doi:10.48550/arxiv.2512.06069 2025

  2. [2]

    L., Chen, X., Ciardi, D., et al

    Akeson, R. L., Chen, X., Ciardi, D., et al. 2013, PASP, 125, 989, doi: 10.1086/672273

    doi:10.1086/672273 2013

  3. [3]

    Ali-Dib, M., Mousis, O., Petit, J.-M., & Lunine, J. I. 2014, ApJ, 785, 125, doi: 10.1088/0004-637X/785/2/125

    doi:10.1088/0004-637x/785/2/125 2014

  4. [4]

    M., Asplund, M., Collet, R., & Leenaarts, J

    Amarsi, A. M., Asplund, M., Collet, R., & Leenaarts, J. 2015, MNRAS, 454, L11, doi: 10.1093/mnrasl/slv122

    doi:10.1093/mnrasl/slv122 2015

  5. [5]

    R., Brown, D

    Anderson, D. R., Brown, D. J. A., Collier Cameron, A., et al. 2014, arXiv e-prints, arXiv:1410.3449, doi: 10.48550/arXiv.1410.3449

    arXiv doi:10.48550/arxiv.1410.3449 2014

  6. [6]

    2014, MNRAS, 443, L89, doi: 10.1093/mnrasl/slu076

    Anglada-Escude, G., Arriagada, P., Tuomi, M., et al. 2014, MNRAS, 443, L89, doi: 10.1093/mnrasl/slu076

    work page doi:10.1093/mnrasl/slu076 2014

  7. [7]

    M., & Grevesse, N

    Asplund, M., Amarsi, A. M., & Grevesse, N. 2021, A&A, 653, A141, doi: 10.1051/0004-6361/202140445

    doi:10.1051/0004-6361/202140445 2021

  8. [8]

    Tuning the Rate of Tightly Packed Systems To Produce Planet Occurrence Trends with Galactic Height

    Ballard, S. 2024, submitted to AJ, arXiv:2409.10485, doi: 10.48550/arXiv.2409.10485

    work page Pith review arXiv doi:10.48550/arxiv.2409.10485 2024

Show all 137 references
  1. [9]

    2019, A&A, 621, A110, doi: 10.1051/0004-6361/201834305

    Barbato, D., Sozzetti, A., Biazzo, K., et al. 2019, A&A, 621, A110, doi: 10.1051/0004-6361/201834305

    2019 doi

  2. [11]

    2019b, AJ, 157, 43, doi: 10.3847/1538-3881/aaf422

    Barkaoui, K., Burdanov, A., Hellier, C., et al. 2019b, AJ, 157, 43, doi: 10.3847/1538-3881/aaf422

    doi

  3. [12]

    L., Hattori, S., Rubenzahl, R

    Behmard, A., Brinkman, C. L., Hattori, S., Rubenzahl, R. A., & Bedell, M. 2025, AJ, 170, 282, doi: 10.3847/1538-3881/ae0e17

    2025 doi

  4. [13]

    2022, MNRAS, 514, 689, doi: 10.1093/mnras/stac1267

    Belokurov, V., & Kravtsov, A. 2022, MNRAS, 514, 689, doi: 10.1093/mnras/stac1267

    2022 doi

  5. [14]

    2020, MNRAS, 496, 1922, doi: 10.1093/mnras/staa1522

    Belokurov, V., Penoyre, Z., Oh, S., et al. 2020, MNRAS, 496, 1922, doi: 10.1093/mnras/staa1522

    2020 doi

  6. [15]

    Bensby, T., Feltzing, S., & Oey, M. S. 2014, A&A, 562, A71, doi: 10.1051/0004-6361/201322631

    2014 doi

  7. [16]

    2005a, ApJS, 157, 402, doi: 10.1086/427924

    Nave, G. 2005a, ApJS, 157, 402, doi: 10.1086/427924

    doi

  8. [17]

    J., Toner, A., Hibbert, A., Webb, J., & Ivarsson, S

    Blackwell-Whitehead, R. J., Toner, A., Hibbert, A., Webb, J., & Ivarsson, S. 2005b, MNRAS, 364, 705, doi: 10.1111/j.1365-2966.2005.09597.x

    2005 doi

  9. [18]

    2016, ARA&A, 54, 529, doi: 10.1146/annurev-astro-081915-023441

    Bland-Hawthorn, J., & Gerhard, O. 2016, ARA&A, 54, 529, doi: 10.1146/annurev-astro-081915-023441

    2016 doi

  10. [19]

    M., Wang, J., Zinn, J

    Boley, K. M., Wang, J., Zinn, J. C., et al. 2021, AJ, 162, 85, doi: 10.3847/1538-3881/ac0e2d

    2021 doi

  11. [20]

    M., Christiansen, J

    Boley, K. M., Christiansen, J. L., Zink, J., et al. 2024, AJ, 168, 128, doi: 10.3847/1538-3881/ad6570

    2024 doi

  12. [21]

    2021, AJ, 161, 230, doi: 10.3847/1538-3881/abec89

    Bortle, A., Fausey, H., Ji, J., et al. 2021, AJ, 161, 230, doi: 10.3847/1538-3881/abec89

    2021 doi

  13. [22]

    2018, ApJL, 867, L3, doi: 10.3847/2041-8213/aae710

    Foreman-Mackey, D. 2018, ApJL, 867, L3, doi: 10.3847/2041-8213/aae710

    2018 doi

  14. [23]

    M., Baliber, N., Bianco, F

    Brown, T. M., Baliber, N., Bianco, F. B., et al. 2013, 125, 1031, doi: 10.1086/673168

    2013 doi

  15. [24]

    M., Tumlinson, J., Geha, M., et al

    Brown, T. M., Tumlinson, J., Geha, M., et al. 2014, ApJ, 796, 91, doi: 10.1088/0004-637X/796/2/91 18J. D. Simon et al

    2014 doi

  16. [25]

    A., Bakos, G

    Buchhave, L. A., Bakos, G. ´A., Hartman, J. D., et al. 2010, ApJ, 720, 1118, doi: 10.1088/0004-637X/720/2/1118

    2010 doi

  17. [26]

    A., Latham, D

    Buchhave, L. A., Latham, D. W., Johansen, A., et al. 2012, Nature, 486, 375, doi: 10.1038/nature11121

    2012 doi

  18. [27]

    E., et al

    Buder, S., Kos, J., Wang, X. E., et al. 2025, PASA, 42, e051, doi: 10.1017/pasa.2025.26

    2025 doi

  19. [28]

    J., et al

    Cadieux, C., Doyon, R., MacDonald, R. J., et al. 2024, ApJL, 970, L2, doi: 10.3847/2041-8213/ad5afa

    2024 doi

  20. [29]

    A., Tenenbaum, P., Twicken, J

    Caldwell, D. A., Tenenbaum, P., Twicken, J. D., et al. 2020, Research Notes of the American Astronomical Society, 4, 201, doi: 10.3847/2515-5172/abc9b3

    2020 doi

  21. [30]

    L., Barclay, T., Swift, J

    Campante, T. L., Barclay, T., Swift, J. J., et al. 2015, ApJ, 799, 170, doi: 10.1088/0004-637X/799/2/170

    2015 doi

  22. [31]

    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

    2003

  23. [32]

    2025, ApJ, 994, 43, doi: 10.3847/1538-4357/ae0cbf

    Murray-Clay, R. 2025, ApJ, 994, 43, doi: 10.3847/1538-4357/ae0cbf

    2025 doi

  24. [33]

    Chiti, A., Frebel, A., Jerjen, H., Kim, D., & Norris, J. E. 2020, ApJ, 891, 8, doi: 10.3847/1538-4357/ab6d72

    2020 doi

  25. [34]

    K., et al

    Chiti, A., Frebel, A., Mardini, M. K., et al. 2021, ApJS, 254, 31, doi: 10.3847/1538-4365/abf73d

    2021 doi

  26. [35]

    2016, ApJ, 823, 102, doi: 10.3847/0004-637X/823/2/102

    Choi, J., Dotter, A., Conroy, C., et al. 2016, ApJ, 823, 102, doi: 10.3847/0004-637X/823/2/102

    2016 doi

  27. [36]

    L., McElroy, D

    Christiansen, J. L., McElroy, D. L., Harbut, M., et al. 2025, PSJ, in press, arXiv:2506.03299, doi: 10.48550/arXiv.2506.03299

    2025 doi arXiv

  28. [37]

    2016, MNRAS, 456, 990, doi: 10.1093/mnras/stv2698

    Ciceri, S., Mancini, L., Southworth, J., et al. 2016, MNRAS, 456, 990, doi: 10.1093/mnras/stv2698

    2016 doi

  29. [38]

    G., Christlieb, N., Qian, Y

    Cohen, J. G., Christlieb, N., Qian, Y. Z., & Wasserburg, G. J. 2003, ApJ, 588, 1082, doi: 10.1086/374269

    2003 doi

  30. [39]

    2019, in American Astronomical Society Meeting Abstracts, Vol

    Collins, K. 2019, in American Astronomical Society Meeting Abstracts, Vol. 233, American Astronomical Society Meeting Abstracts #233, 140.05

    2019

  31. [40]

    A., Kielkopf, J

    Collins, K. A., Kielkopf, J. F., Stassun, K. G., & Hessman, F. V. 2017, AJ, 153, 77, doi: 10.3847/1538-3881/153/2/77

    2017 doi

  32. [41]

    2025, AJ, 170, 226, doi: 10.3847/1538-3881/adfc6a

    Coulombe, L.-P., Benneke, B., Krissansen-Totton, J., et al. 2025, AJ, 170, 226, doi: 10.3847/1538-3881/adfc6a

    2025 doi

  33. [42]

    M., Skrutskie, M

    Cutri, R. M., Skrutskie, M. F., van Dyk, S., et al. 2003, 2MASS All Sky Catalog of point sources

    2003

  34. [43]

    M., Wright, E

    Cutri, R. M., Wright, E. L., Conrow, T., et al. 2021,, VizieR On-line Data Catalog: II/328. Originally published in: IPAC/Caltech (2013)

    2021

  35. [44]

    I., & Johnson, J

    Dawson, R. I., & Johnson, J. A. 2018, ARA&A, 56, 175, doi: 10.1146/annurev-astro-081817-051853 de Leon, J. P., Livingston, J., Endl, M., et al. 2021, MNRAS, 508, 195, doi: 10.1093/mnras/stab2305 Delgado Mena, E., Adibekyan, V., Santos, N. C., et al. 2021, A&A, 655, A99, doi: 1...

    2018 doi

  36. [45]

    Demarque, P., Woo, J.-H., Kim, Y.-C., & Yi, S. K. 2004, ApJS, 155, 667, doi: 10.1086/424966

    2004 doi

  37. [46]

    2025, submitted to ApJ, arXiv:2508.16805, doi: 10.48550/arXiv.2508.16805

    DiTomasso, V., Charbonneau, D., Vanderburg, A., et al. 2025, submitted to ApJ, arXiv:2508.16805, doi: 10.48550/arXiv.2508.16805

    2025 doi arXiv

  38. [47]

    W., Rodr´ ıguez Mart´ ınez, R., et al

    DiTomasso, V., Yee, S. W., Rodr´ ıguez Mart´ ınez, R., et al. 2026, submitted to AJ

    2026

  39. [48]

    2008, ApJS, 178, 89, doi: 10.1086/589654

    Dotter, A., Chaboyer, B., Jevremovi´ c, D., et al. 2008, ApJS, 178, 89, doi: 10.1086/589654

    2008 doi

  40. [49]

    2024, Nature, 625, 51, doi: 10.1038/s41586-023-06849-0

    Dyrek, A., Min, M., Decin, L., et al. 2024, Nature, 625, 51, doi: 10.1038/s41586-023-06849-0

    2024 doi

  41. [50]

    S., & Agol, E

    Eastman, J., Gaudi, B. S., & Agol, E. 2013, PASP, 125, 83, doi: 10.1086/669497

    2013 doi

  42. [51]

    D., Rodriguez, J

    Eastman, J. D., Rodriguez, J. E., Agol, E., et al. 2019, arXiv e-prints, arXiv:1907.09480, doi: 10.48550/arXiv.1907.09480

    2019 doi arXiv

  43. [52]

    El-Badry, K., Rix, H.-W., & Heintz, T. M. 2021, MNRAS, 506, 2269, doi: 10.1093/mnras/stab323

    2021 doi

  44. [53]

    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

  45. [54]

    P., Santos, N

    Faria, J. P., Santos, N. C., Figueira, P., et al. 2016, A&A, 589, A25, doi: 10.1051/0004-6361/201527522

    2016 doi

  46. [55]

    2003, A&A, 397, L1, doi: 10.1051/0004-6361:20021661

    Feltzing, S., Bensby, T., & Lundstr¨ om, I. 2003, A&A, 397, L1, doi: 10.1051/0004-6361:20021661

    2003 doi

  47. [56]

    2025, submitted to ApJ, arXiv:2512.17072, doi: 10.48550/arXiv.2512.17072 F˝ ur´ esz, G

    Ferreira, T., Yana Galarza, J., Reggiani, H., et al. 2025, submitted to ApJ, arXiv:2512.17072, doi: 10.48550/arXiv.2512.17072 F˝ ur´ esz, G. 2008, PhD thesis, University of Szeged, Hungary

    2025 doi

  48. [57]

    A., & Valenti, J

    Fischer, D. A., & Valenti, J. 2005, ApJ, 622, 1102, doi: 10.1086/428383 Gaia Collaboration, Prusti, T., de Bruijne, J. H. J., et al. 2016, A&A, 595, A1, doi: 10.1051/0004-6361/201629272 Gaia Collaboration, Smart, R. L., Sarro, L. M., et al. 2021, A&A, 649, A6, doi: 10.1051/000...

    2005 doi

  49. [58]

    2019, ApJ, 887, 93, doi: 10.3847/1538-4357/ab5362

    Finkbeiner, D. 2019, ApJ, 887, 93, doi: 10.3847/1538-4357/ab5362

    2019 doi

  50. [59]

    J., Espinoza, N., et al

    Gressier, A., MacDonald, R. J., Espinoza, N., et al. 2025, AJ, 169, 57, doi: 10.3847/1538-3881/ad97bf

    2025 doi

  51. [60]

    2022, A&A, 668, A29, doi: 10.1051/0004-6361/202244077 A Transiting Giant Planet Around a Metal-Poor Star19

    Grieves, N., Bouchy, F., Ulmer-Moll, S., et al. 2022, A&A, 668, A29, doi: 10.1051/0004-6361/202244077 A Transiting Giant Planet Around a Metal-Poor Star19

    2022 doi

  52. [61]

    M., Seager, S., Huang, C

    Guerrero, N. M., Seager, S., Huang, C. X., et al. 2021, ApJS, 254, 39, doi: 10.3847/1538-4365/abefe1

    2021 doi

  53. [62]

    Hallatt, T., & Lee, E. J. 2025, ApJ, 979, 120, doi: 10.3847/1538-4357/ad9aa1

    2025 doi

  54. [63]

    R., Collier Cameron, A., et al

    Hellier, C., Anderson, D. R., Collier Cameron, A., et al. 2014, MNRAS, 440, 1982, doi: 10.1093/mnras/stu410

    2014 doi

  55. [64]

    2017, A&A, 603, A123, doi: 10.1051/0004-6361/201629696

    Helling, C., Tootill, D., Woitke, P., & Lee, E. 2017, A&A, 603, A123, doi: 10.1051/0004-6361/201629696

    2017 doi

  56. [65]

    R., Timmes, F

    Hinkel, N. R., Timmes, F. X., Young, P. A., Pagano, M. D., & Turnbull, M. C. 2014, AJ, 148, 54, doi: 10.1088/0004-6256/148/3/54

    2014 doi

  57. [66]

    J., Kitzmann, D., Morris, B

    Hoeijmakers, H. J., Kitzmann, D., Morris, B. M., et al. 2024, A&A, 685, A139, doi: 10.1051/0004-6361/202244968

    2024 doi

  58. [67]

    Ciardi, D. R. 2011, AJ, 142, 19, doi: 10.1088/0004-6256/142/1/19

    2011 doi

  59. [68]

    2024, Nature, 630, 609, doi: 10.1038/s41586-024-07432-x

    Hu, R., Bello-Arufe, A., Zhang, M., et al. 2024, Nature, 630, 609, doi: 10.1038/s41586-024-07432-x

    2024 doi

  60. [69]

    X., Vanderburg, A., P´ al, A., et al

    Huang, C. X., Vanderburg, A., P´ al, A., et al. 2020a, Research Notes of the American Astronomical Society, 4, 204, doi: 10.3847/2515-5172/abca2e

    doi

  61. [70]

    X., Vanderburg, A., P´ al, A., et al

    Huang, C. X., Vanderburg, A., P´ al, A., et al. 2020b, Research Notes of the American Astronomical Society, 4, 206, doi: 10.3847/2515-5172/abca2d

    doi

  62. [71]

    A., Zasowski, G., et al

    Imig, J., Holtzman, J. A., Zasowski, G., et al. 2025, ApJ, 990, 203, doi: 10.3847/1538-4357/adf723

    2025 doi

  63. [72]

    M., Twicken, J

    Jenkins, J. M., Twicken, J. D., McCauliff, S., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9913, Software and Cyberinfrastructure for Astronomy IV, ed. G. Chiozzi & J. C. Guzman, 99133E, doi: 10.1117/12.2233418

    2016 doi

  64. [73]

    2013,, Astrophysics Source Code Library http://ascl.net/1306.007

    Jensen, E. 2013,, Astrophysics Source Code Library http://ascl.net/1306.007

    2013

  65. [74]

    L., & Li, H

    Johnson, J. L., & Li, H. 2012, ApJ, 751, 81, doi: 10.1088/0004-637X/751/2/81

    2012 doi

  66. [75]

    C., Schmidt, B

    Keller, S. C., Schmidt, B. P., Bessell, M. S., et al. 2007, PASA, 24, 1, doi: 10.1071/AS07001

    2007 doi

  67. [76]

    M.-R., Bean, J

    Kempton, E. M.-R., Bean, J. L., Louie, D. R., et al. 2018, PASP, 130, 114401, doi: 10.1088/1538-3873/aadf6f

    2018 doi

  68. [77]

    Z., Fuhr, J

    Klose, J. Z., Fuhr, J. R., & Wiese, W. L. 2002, Journal of Physical and Chemical Reference Data, 31, 217, doi: 10.1063/1.1448482

    2002 doi

  69. [78]

    E., Wood, M

    Lawler, J. E., Wood, M. P., Den Hartog, E. A., et al. 2014, ApJS, 215, 20, doi: 10.1088/0067-0049/215/2/20

    2014 doi

  70. [79]

    C., Park, M

    Lee, B. C., Park, M. G., Lee, S. M., et al. 2015, A&A, 584, A79, doi: 10.1051/0004-6361/201527076 Lightkurve Collaboration, Cardoso, J. V. d. M., Hedges, C., et al. 2018,, Astrophysics Source Code Library, record ascl:1812.013 http://ascl.net/1812.013

    2015 doi

  71. [80]

    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

  72. [81]

    R., Mullens, E., Alderson, L., et al

    Louie, D. R., Mullens, E., Alderson, L., et al. 2025, AJ, 169, 86, doi: 10.3847/1538-3881/ad9688

    2025 doi

  73. [82]

    T., Bovy, J., Schiavon, R

    Mackereth, J. T., Bovy, J., Schiavon, R. P., et al. 2017, MNRAS, 471, 3057, doi: 10.1093/mnras/stx1774

    2017 doi

  74. [83]

    V., & Lunine, J

    Madhusudhan, N., Mousis, O., Johnson, T. V., & Lunine, J. I. 2011, ApJ, 743, 191, doi: 10.1088/0004-637X/743/2/191

    2011 doi

  75. [84]

    2016, MNRAS, 461, 1053, doi: 10.1093/mnras/stw1386

    Mancini, L., Giordano, M., Molli` ere, P., et al. 2016, MNRAS, 461, 1053, doi: 10.1093/mnras/stw1386

    2016 doi

  76. [85]

    F., Starkenburg, E., Yuan, Z., et al

    Martin, N. F., Starkenburg, E., Yuan, Z., et al. 2024, A&A, 692, A115, doi: 10.1051/0004-6361/202347633

    2024 doi

  77. [86]

    2023, MNRAS, 522, 3217, doi: 10.1093/mnras/stad1177

    Martos, G., Mel´ endez, J., Rathsam, A., & Carvalho Silva, G. 2023, MNRAS, 522, 3217, doi: 10.1093/mnras/stad1177

    2023 doi

  78. [87]

    Mateu, C., & Vivas, A. K. 2018, MNRAS, 479, 211, doi: 10.1093/mnras/sty1373

    2018 doi

  79. [88]

    H., Harbeck, D.-R., et al

    McCully, C., Volgenau, N. H., Harbeck, D.-R., et al. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10707, Proc. SPIE, 107070K, doi: 10.1117/12.2314340

    2018 doi

  80. [89]

    1998, AJ, 115, 1640, doi: 10.1086/300289

    McWilliam, A. 1998, AJ, 115, 1640, doi: 10.1086/300289

    1998 doi

  81. [90]

    B., Ahrer, E.-M., et al

    Meech, A., Claringbold, A. B., Ahrer, E.-M., et al. 2025, MNRAS, 539, 1381, doi: 10.1093/mnras/staf530 Mel´ endez, J., Ram´ ırez, I., Karakas, A. I., et al. 2014, ApJ, 791, 14, doi: 10.1088/0004-637X/791/1/14

    2025 doi

  82. [91]

    M., & Badenes, C

    Moe, M., Kratter, K. M., & Badenes, C. 2019, ApJ, 875, 61, doi: 10.3847/1538-4357/ab0d88

    2019 doi

  83. [92]

    C., Sousa, S., et al

    Mortier, A., Santos, N. C., Sousa, S., et al. 2013, A&A, 551, A112, doi: 10.1051/0004-6361/201220707

    2013 doi

  84. [93]

    C., Sozzetti, A., et al

    Mortier, A., Santos, N. C., Sozzetti, A., et al. 2012, A&A, 543, A45, doi: 10.1051/0004-6361/201118651

    2012 doi

  85. [94]

    D., Bryson, S

    Morton, T. D., Bryson, S. T., Coughlin, J. L., et al. 2016, ApJ, 822, 86, doi: 10.3847/0004-637X/822/2/86

    2016 doi

  86. [95]

    Narita, N., Fukui, A., Kusakabe, N., et al. 2019, J. Astron. Telesc. Instruments, Syst., 5, 015001, doi: 10.1117/1.JATIS.5.1.015001

    2019 doi

  87. [96]

    R., et al

    Parviainen, H., Palle, E., Zapatero-Osorio, M. R., et al. 2020, A&A, 633, A28, doi: 10.1051/0004-6361/201935958

    2020 doi

  88. [97]

    K., Cargile, P

    Pass, E. K., Cargile, P. A., DiTomasso, V., et al. 2025, ApJS, in press, arXiv:2506.18961, doi: 10.48550/arXiv.2506.18961

    2025 doi

  89. [98]

    A., Brandeker, A., Kitzmann, D., et al

    Patel, J. A., Brandeker, A., Kitzmann, D., et al. 2024, A&A, 690, A159, doi: 10.1051/0004-6361/202450748

    2024 doi

  90. [99]

    V., Kaminsky, B

    Pavlenko, Y. V., Kaminsky, B. M., Jenkins, J. S., et al. 2019, A&A, 621, A112, doi: 10.1051/0004-6361/201834138

    2019 doi

  91. [100]

    Penoyre, Z., Belokurov, V., & Evans, N. W. 2022, MNRAS, 513, 2437, doi: 10.1093/mnras/stac959 20J. D. Simon et al

    2022 doi

  92. [101]

    A., Marcy, G

    Petigura, E. A., Marcy, G. W., Winn, J. N., et al. 2018, AJ, 155, 89, doi: 10.3847/1538-3881/aaa54c

    2018 doi

  93. [102]

    Price-Whelan, A. M. 2017, The Journal of Open Source Software, 2, 388, doi: 10.21105/joss.00388

    2017 doi

  94. [103]

    X., & McWilliam, A

    Prochaska, J. X., & McWilliam, A. 2000, ApJL, 537, L57, doi: 10.1086/312749

    2000 doi

  95. [104]

    McWilliam, A., & Wolfe, A. M. 2000, AJ, 120, 2513, doi: 10.1086/316818

    2000 doi

  96. [105]

    N., White, R

    Quinn, S. N., White, R. J., Latham, D. W., et al. 2012, ApJL, 756, L33, doi: 10.1088/2041-8205/756/2/L33 Ram´ ırez, I., Mel´ endez, J., Bean, J., et al. 2014, A&A, 572, A48, doi: 10.1051/0004-6361/201424244

    2012 doi

  97. [106]

    R., Winn, J

    Ricker, G. R., Winn, J. N., Vanderspek, R., et al. 2015, Journal of Astronomical Telescopes, Instruments, and Systems, 1, 014003, doi: 10.1117/1.JATIS.1.1.014003

    2015 doi

  98. [107]

    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

  99. [108]

    C., Reyl´ e, C., Fliri, J., et al

    Robin, A. C., Reyl´ e, C., Fliri, J., et al. 2014, A&A, 569, A13, doi: 10.1051/0004-6361/201423415

    2014 doi

  100. [109]

    E., Quinn, S

    Rodriguez, J. E., Quinn, S. N., Zhou, G., et al. 2021, AJ, 161, 194, doi: 10.3847/1538-3881/abe38a Rodr´ ıguez Mart´ ınez, R., Martin, D. V., Gaudi, B. S., et al. 2023, AJ, 166, 137, doi: 10.3847/1538-3881/aced9a

    2021 doi

  101. [110]

    Saha, S., & Jenkins, J. S. 2025, ApJL, 994, L39, doi: 10.3847/2041-8213/ae1c1c

    2025 doi

  102. [111]

    1993, ApJ, 414, 580, doi: 10.1086/173105

    Salaris, M., Chieffi, A., & Straniero, O. 1993, ApJ, 414, 580, doi: 10.1086/173105

    1993 doi

  103. [112]

    C., Mayor, M., Bonfils, X., et al

    Santos, N. C., Mayor, M., Bonfils, X., et al. 2011, A&A, 526, A112, doi: 10.1051/0004-6361/201015494

    2011 doi

  104. [113]

    J., Finkbeiner, D

    Schlegel, D. J., Finkbeiner, D. P., & Davis, M. 1998, ApJ, 500, 525, doi: 10.1086/305772

    1998 doi

  105. [114]

    E., Bieryla, A., et al

    Schulte, J., Rodriguez, J. E., Bieryla, A., et al. 2024, AJ, 168, 32, doi: 10.3847/1538-3881/ad4a57

    2024 doi

  106. [115]

    E., Latham, D

    Schulte, J., Rodriguez, J. E., Latham, D. W., et al. 2025, MNRAS, 543, 292, doi: 10.1093/mnras/staf1455

    2025 doi

  107. [116]

    J., Howell, S

    Scott, N. J., Howell, S. B., Horch, E. P., & Everett, M. E. 2018, PASP, 130, 054502, doi: 10.1088/1538-3873/aab484

    2018 doi

  108. [117]

    J., Howell, S

    Scott, N. J., Howell, S. B., Gnilka, C. L., et al. 2021, Frontiers in Astronomy and Space Sciences, 8, 138, doi: 10.3389/fspas.2021.716560

    2021 doi

  109. [118]

    2024, A&A, 690, A107, doi: 10.1051/0004-6361/202449669

    Shejeelammal, J., Mel´ endez, J., Rathsam, A., & Martos, G. 2024, A&A, 690, A107, doi: 10.1051/0004-6361/202449669

    2024 doi

  110. [119]

    K., Faedi, F., Barros, S

    Simpson, E. K., Faedi, F., Barros, S. C. C., et al. 2011, AJ, 141, 8, doi: 10.1088/0004-6256/141/1/8

    2011 doi

  111. [120]

    Sneden, C. A. 1973, PhD thesis, THE UNIVERSITY OF TEXAS AT AUSTIN

    1973

  112. [121]

    2011, MNRAS, 417, 2166, doi: 10.1111/j.1365-2966.2011.19399.x

    Southworth, J. 2011, MNRAS, 417, 2166, doi: 10.1111/j.1365-2966.2011.19399.x

    2011 doi

  113. [122]

    W., et al

    Sozzetti, A., Torres, G., Latham, D. W., et al. 2009, ApJ, 697, 544, doi: 10.1088/0004-637X/697/1/544

    2009 doi

  114. [123]

    2017, MNRAS, 471, 2587, doi: 10.1093/mnras/stx1068

    Starkenburg, E., Martin, N., Youakim, K., et al. 2017, MNRAS, 471, 2587, doi: 10.1093/mnras/stx1068

    2017 doi

  115. [124]

    H., & Fur´ esz, G

    Szentgyorgyi, A. H., & Fur´ esz, G. 2007, in Revista Mexicana de Astronomia y Astrofisica Conference Series, Vol. 28, Revista Mexicana de Astronomia y Astrofisica Conference Series, ed. S. Kurtz, 129–133

    2007

  116. [125]

    2018, PASJ, 70, 59, doi: 10.1093/pasj/psy052

    Takarada, T., Sato, B., Omiya, M., et al. 2018, PASJ, 70, 59, doi: 10.1093/pasj/psy052

    2018 doi

  117. [126]

    P., & Vogelaar, M

    Terlouw, J. P., & Vogelaar, M. G. R. 2015, Kapteyn Package, version 2.3, Kapteyn Astronomical Institute, Groningen

    2015

  118. [127]

    Vanderburg, A., & Johnson, J. A. 2014, PASP, 126, 948, doi: 10.1086/678764

    2014 doi

  119. [128]

    2017, A&A, 606, A38, doi: 10.1051/0004-6361/201730471

    Villaver, E., Niedzielski, A., Wolszczan, A., et al. 2017, A&A, 606, A38, doi: 10.1051/0004-6361/201730471

    2017 doi

  120. [129]

    2025, AJ, 169, 117, doi: 10.3847/1538-3881/ada143

    Vissapragada, S., & Behmard, A. 2025, AJ, 169, 117, doi: 10.3847/1538-3881/ada143

    2025 doi

  121. [130]

    R., & Sing, D

    Wakeford, H. R., & Sing, D. K. 2015, A&A, 573, A122, doi: 10.1051/0004-6361/201424207

    2015 doi

  122. [131]

    2025, MNRAS, 541, 2459, doi: 10.1093/mnras/staf829

    Weeks, A., Huber, D., Stokholm, A., et al. 2025, MNRAS, 541, 2459, doi: 10.1093/mnras/staf829

    2025 doi

  123. [132]

    J., Benisty, M., & Andrews, S

    Winter, A. J., Benisty, M., & Andrews, S. M. 2024, ApJL, 972, L9, doi: 10.3847/2041-8213/ad6d5d

    2024 doi

  124. [133]

    L., Eisenhardt, P

    Wright, E. L., Eisenhardt, P. R. M., Mainzer, A. K., et al. 2010, AJ, 140, 1868, doi: 10.1088/0004-6256/140/6/1868

    2010 doi

  125. [134]

    2022, Nature, 603, 599, doi: 10.1038/s41586-022-04496-5

    Xiang, M., & Rix, H.-W. 2022, Nature, 603, 599, doi: 10.1038/s41586-022-04496-5

    2022 doi

  126. [135]

    2025, Nature Astronomy, 9, 101, doi: 10.1038/s41550-024-02382-w Yana Galarza, J., L´ opez-Valdivia, R., Mel´ endez, J., &

    Xiang, M., Rix, H.-W., Yang, H., et al. 2025, Nature Astronomy, 9, 101, doi: 10.1038/s41550-024-02382-w Yana Galarza, J., L´ opez-Valdivia, R., Mel´ endez, J., &

    2025 doi

  127. [136]

    2021a, ApJ, 922, 129, doi: 10.3847/1538-4357/ac2362 Yana Galarza, J., L´ opez-Valdivia, R., Lorenzo-Oliveira, D., et al

    Lorenzo-Oliveira, D. 2021a, ApJ, 922, 129, doi: 10.3847/1538-4357/ac2362 Yana Galarza, J., L´ opez-Valdivia, R., Lorenzo-Oliveira, D., et al. 2021b, MNRAS, 504, 1873, doi: 10.1093/mnras/stab987 Yana Galarza, J., Reggiani, H., Ferreira, T., et al. 2024, ApJ, 974, 122, doi: 10.3...

    2024 doi

  128. [137]

    2001, ApJS, 136, 417, doi: 10.1086/321795

    Yi, S., Demarque, P., Kim, Y.-C., et al. 2001, ApJS, 136, 417, doi: 10.1086/321795

    2001 doi

  129. [138]

    K., Hardegree-Ullman, K

    Zink, J. K., Hardegree-Ullman, K. K., Christiansen, J. L., et al. 2023, AJ, 165, 262, doi: 10.3847/1538-3881/acd24c

    2023 doi

Pith tools

Reviewed July 13, 2026 · model on record in the stance chip above.