Pith. sign in

REVIEW 2 major objections 3 minor 150 references

Precise Asteroseismic Ages for the Helmi Streams

T0 review · 2 major / 3 minor · reviewed 2026-08-06 · deepseek-v4-flash

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

Pith's one-line read This paper reports precise asteroseismic ages for two Helmi stream red giants, 11.16 and 12.52 billion years, and shows that global asteroseismic parameters underestimate ages of metal-poor giants.

desk verdict One solid age (HD 128279), one conditional age (HD 175305), and a useful confirmation of scaling-relation biases—worth peer review despite the unresolved evolutionary-state question. read the letter →

arxiv 2507.01091 v1 pith:EI6TDFE4 submitted 2025-07-01 astro-ph.SR astro-ph.GA

Christopher J. Lindsay , Marc Hon , J. M. Joel Ong , Rafael A. García , Dinil B. Palakkatharappil , Jie Yu , Tanda Li , Tomás Ruiz-Lara
show 1 more author
Amina Helmi
This is my paper · ORCID
classification astro-ph.SRastro-ph.GA
keywords asteroseismologyredgiantstarsHelmistreamsGalacticarchaeologystellaragesmetal-poorTESSmixedmodes
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

This paper reports the first detailed asteroseismic ages for two confirmed members of the Helmi streams, the shredded remains of a dwarf galaxy that merged with the Milky Way. By fitting the individual oscillation-mode frequencies of the red giants HD 175305 and HD 128279, the authors obtain ages of $ au = 11.16 \pm 0.91$ Gyr and $ au = 12.52 \pm 1.05$ Gyr. These ages place the start of star formation in the stream's progenitor at least 12 billion years ago, in line with earlier isochrone-based star-formation histories. The same analysis shows that ages computed from global asteroseismic parameters ($\Delta\nu$ and $\nu_{\rm max}$) are much younger and underestimate true ages for metal-poor, $\alpha$-enhanced giants. A careful reader would care because precise ages for individual accreted stars turn a kinematic debris stream into a dated assembly story for the Milky Way's halo.

What carries the argument

The load-bearing tool is detailed asteroseismic modeling of individual oscillation mode frequencies, especially the mixed $\ell=1$ modes that couple pressure modes in the outer envelope to gravity modes in the core and therefore carry age information. The authors generate stellar evolutionary tracks, compute mode frequencies, apply a two-term surface correction, and use a differential-evolution optimizer to minimize a combined spectroscopic and seismic $\chi^2$. The gravity-mode period spacing $\Delta\Pi_1$ is used as a consistency check on evolutionary state. This machinery converts faint oscillation peaks in TESS power spectra into masses, radii, and ages that disagree sharply with global-scaling-relation results.

What would settle it

Observe HD 175305 with a longer TESS baseline and measure its gravity-mode period spacing $\Delta\Pi_1$: a value near 275 s would show it is core-helium burning and invalidate the 11.16 Gyr age, while a value near 68 s would confirm the red-giant-branch interpretation. A second decisive test is an independent stellar radius from interferometry consistent with the detailed model radius (~7.4 $R_\odot$) rather than the larger global-scaling radius.

Watch

Extended reading notes

Core claim

The paper's central claim is that two metal-poor red giants in the Helmi streams can be precisely dated by modeling their individual radial, dipole, and quadrupole oscillation frequencies along with spectroscopic temperatures, luminosities, and metallicities. The best-fit models give $\tau = 11.16 \pm 0.91$ Gyr for HD 175305 and $\tau = 12.52 \pm 1.05$ Gyr for HD 128279, with the older star more metal-poor and more $\alpha$-enhanced. The authors argue these ages are consistent with the stream's known star-formation history and chemical-abundance spread, and that the older age bounds when the progenitor first formed stars to at least ~12 Gyr ago. They further claim that grid-based ages using only global asteroseismic parameters are severely underestimated (6.4 Gyr versus 11.2 Gyr for HD 175305, and 4.5 Gyr versus 12.5 Gyr for HD 128279), so individual mode frequencies are necessary for age-dating metal-poor giants.

Load-bearing premise

HD 175305 is a first-ascent red giant burning hydrogen in a shell; if it is actually a core-helium-burning clump star, the reported 11.16 Gyr age collapses because such a star would be much younger.

Editorial extensions

If this is right

  • The Helmi streams' progenitor must have begun forming stars at least ~12 Gyr ago, predating its merger with the Milky Way 5–8 Gyr ago.
  • Ages of metal-poor, $\alpha$-enhanced red giants derived from global asteroseismic scaling relations are systematically too young, so future halo archaeology needs individual-mode modeling for such stars.
  • The older, more metal-poor star being more $\alpha$-enhanced supports a picture where the stream's chemical evolution ran from an $\alpha$-rich, low-metallicity population to a less $\alpha$-rich, more metal-rich one.
  • The ~50 bright Helmi stream giants visible to TESS become plausible targets for turning the stream's star-formation history into a dated sequence.
  • Precise asteroseismic ages for r-process-enhanced stream members like HD 175305 could calibrate radioactive cosmochronometry ages.

Reading between the lines

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

  • If HD 175305 is actually a secondary-clump helium-burning star, its reported 11.16 Gyr age would be too young, and the stream-age lower bound would rest on HD 128279 alone; longer TESS observations of its period spacing could settle this.
  • The $f_{\nu_{\rm max}}$ values near 1.05–1.11 imply the standard $\nu_{\rm max}$ scaling relation overestimates surface gravity for these stars; extending individual-mode fits to a larger metal-poor sample could turn this offset into a metallicity-dependent correction.
  • The age-metallicity trend across the two stars lines up with the 'inverted knee' in [Mg/Fe] versus [Fe/H] seen spectroscopically, so dating more stream members could test whether that knee is a time sequence rather than a spatial abundance pattern.
  • A testable extension is to model the ~50 bright Helmi giant candidates with TESS sectors to map the stream's age-[Fe/H] plane and compare with dwarf-galaxy chemical-evolution models.
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 / 3 minor

Summary. The paper reports detailed asteroseismic modeling of two bright red giants in the Helmi streams, HD 175305 and HD 128279, using TESS photometry. Individual oscillation mode frequencies are extracted with TACO and fitted with MESA/GYRE evolutionary models, with effective temperature, luminosity, and chemical abundances as external constraints. The best-fit ages are τ = 11.16 ± 0.91 Gyr for HD 175305 and τ = 12.52 ± 1.05 Gyr for HD 128279. The authors argue these ages match prior isochrone-based star-formation histories of the Helmi streams, and they further show that global asteroseismic scaling relations would give younger ages and larger masses for these metal-poor, α-enhanced stars. The central conclusions are that the Helmi-stream progenitor formed stars at least ~12 Gyr ago and that global asteroseismic parameters systematically bias ages for this stellar population.

Significance. If the ages are correct, this is the first detailed asteroseismic dating of individual Helmi-stream members, providing a quantitative anchor for the progenitor's star-formation history and strengthening the case that the stream formed more than 12 Gyr ago. The paper also makes a useful contribution to the growing body of evidence that global asteroseismic scaling relations overestimate masses and underestimate ages for metal-poor giants; that claim is supported independently by HD 128279 and by previous work. The manuscript is unusually transparent: mode-frequency tables are provided, the optimization and cost-function steps are detailed in the appendix, and the MESA/GYRE inlists and tracks are archived on Zenodo. The period-spacing analysis is a valuable cross-check even where, as for HD 175305, it does not uniquely determine the evolutionary state. These strengths make the paper well positioned for the field, but the conditional nature of the HD 175305 age needs to be addressed before the two-star conclusions can be taken at face value.

major comments (2)
  1. [§2.2 and §5.4] The age of HD 175305 is conditional on the assumption that it is a first-ascent red giant branch star, and the paper's own period-spacing analysis shows that this assumption is not secure. Section 5.4 reports that the PBJam/reggae posterior has a global maximum at ΔΠ1 ≈ 275 s, which is the signature of core-helium burning, with only a local maximum near 68 s consistent with first-ascent RGB; the authors explicitly state that they cannot definitively rule out a secondary clump. Because the asteroseismic optimization in Section 3 and Appendix A searches only first-ascent RGB evolutionary tracks, the reported τ = 11.16 ± 0.91 Gyr is the age of the best RGB model conditional on an unverified evolutionary state. If HD 175305 is a secondary-clump helium-burning star, it would be much younger unless its structure results from a merger or mass-transfer event. This affects the abstract's two-star age set and the statement that the results 'reinforce the hypothesis' of a ≥12 Gyr progenitor, although the ≥12 Gyr conclusion survives through HD 128279 alone. I recommend that the authors either quantify the secondary-clump interpretation (for example, by modeling HD 175305 with core-helium-burning tracks and reporting the resulting age and posterior weight) or explicitly restrict the headline conclusion to HD 128279 and present the HD 175305 age as conditional on the RGB assumption.
  2. [§5.3, Figure 8] The best-fit model radius for HD 175305 is 7.40 ± 0.07 R⊙, which is more than 5σ smaller than the CHARA interferometric radius of 8.2 ± 0.11 R⊙ reported in §5.3. The paper attributes this to the surface-term correction removing sensitivity to the near-surface layers, but this discrepancy raises a concrete question about the robustness of the detailed-model inferences, including the age. Since the interferometric radius also implies a lower effective temperature (Teff = 4850 ± 118 K) than the adopted spectroscopic value, the authors should test whether including the interferometric radius or the interferometric Teff as an additional constraint changes the best-fit mass and age of HD 175305. At minimum, the paper should state explicitly how the reported age uncertainties incorporate this external radius disagreement.
minor comments (3)
  1. [§2.2] The text says 'we assume that both HD 17305 and HD 128279 are first ascent red giant branch stars'; 'HD 17305' should be 'HD 175305'.
  2. [§5.4, Eq. (6)] The integral in Eq. (6) is typeset as 'Z core N r dr' in the draft; this should be ∫(N/r) dr over the core to match the standard definition of the buoyancy integral.
  3. [§5.3] The fνmax values (1.05 for HD 175305 and 1.11 for HD 128279) are quoted without uncertainties; propagating the uncertainties on νmax, mass, radius, and Teff would make the comparison with previous work more quantitative.

Circularity Check

1 steps flagged · score 3.0 of 10

Partial circularity: the old age of HD 175305 is conditioned on a first-ascent RGB assumption motivated by the old-stream prior it is then used to reinforce; the independent HD 128279-based lower bound is not circular.

  1. self definitional [Section 2.2 and Section 5.4 (evolutionary-state assumption and period-spacing caveat)]
    "This assumption is made based on the two stars’ kinematic membership in the relatively old Helmi streams structure and their low metallicities. ... we cannot definitively rule out HD 175305 being a core Helium burning star based solely on the asteroseismic data. If HD 175305 was a secondary clump helium burning star, it would be much younger."

    The modeling pipeline optimizes only first-ascent RGB tracks, and the RGB choice is justified by the prior that the stars belong to the old Helmi streams. For HD 175305, the paper's own PBJam/reggae analysis finds a global period-spacing maximum near 275 s, a core-He burning signature, and only a local maximum near 68 s, consistent with RGB, so the 11.16 Gyr best-fit age is an output of the assumed evolutionary state rather than an independent measurement. Using that conditional age to reinforce the hypothesis that the Helmi streams' progenitor must have existed at least 12 Gyr ago therefore leans on the prior it claims to confirm.

full rationale

The core fitting procedure is not circular: MESA/GYRE models are optimized against individual mode frequencies, Teff, luminosity, and [Fe/H], with the age emerging from the best-fit model rather than being a fitted input. The global-versus-detailed asteroseismology comparison is an independent check using a custom grid and Asfgrid. Self-citations (Lindsay et al. 2024 cost function, Ong & Basu 2020 mode isolation, Hon et al. 2024 modelflows) are methodological and non-load-bearing. The one circular step is the use of the old-stream membership to justify the first-ascent RGB assumption for HD 175305, which then produces the old age used to reinforce the stream's old age; the paper is transparent about this limitation. Because HD 128279 independently anchors the old-age conclusion, the central claim retains independent content, and no self-citation chain or fitted-parameter renaming is present. Score 3 reflects this partial, localized circularity rather than wholesale reduction of the derivation to its inputs.

Assumptions & free parameters 5 free parameters · 7 assumptions · 0 invented entities

The central age determinations rest on a chain of modeling assumptions: standard stellar evolution physics in MESA, the validity of the surface-term correction, the adopted spectroscopic parameters (especially Teff), and the assignment of both stars to the first-ascent RGB. The first-ascent assignment for HD 175305 is a prior, not a measurement. No new physical entities are introduced.

free parameters (5)
  • Initial mass M0 = 0.83 M_sun (HD 175305), 0.77 M_sun (HD 128279)
    Varied in the differential evolution optimization over [0.7, 1.0] M_sun; the age is highly sensitive to this parameter.
  • Initial helium abundance Y0 = 0.25 (HD 175305), 0.26 (HD 128279)
    Varied over [0.245, 0.27]; influences the main-sequence lifetime and hence the age.
  • Initial metal-to-hydrogen ratio f = Z0/X0 = Model [Fe/H] = -1.46 (HD 175305), -2.17 (HD 128279)
    Varied over f in [0.0001, 0.003]; sets the opacity and evolution timescale.
  • Convective mixing length alpha_mlt = 1.80 (HD 175305), 1.97 (HD 128279)
    Varied over [1.6, 2.0]; changes Teff of the model and thus the inferred radius and age.
  • Surface-term correction coefficients (Ball & Gizon 2014) = a, b (not tabulated, fitted to the ℓ=0 modes)
    Free coefficients in the two-term surface correction; they affect the seismic chi-square and therefore the model selection and age.
assumptions (7)
  • domain assumption MESA stellar models with the chosen input physics (element diffusion, exponential overshoot, gray atmosphere) adequately represent metal-poor red giants.
    Invoked throughout Section 3 and Appendix A; the age is a direct output of these models.
  • domain assumption The two-term Ball & Gizon (2014) surface correction is valid for low-metallicity giants.
    Used in Section 3 and Appendix A to compare model and observed frequencies; if the correction is inadequate, the seismic fit and derived parameters shift.
  • domain assumption The spectroscopic parameters from Ishigaki et al. (2012) are accurate for both stars.
    Teff, [Fe/H], and [alpha/Fe] from this source are inputs to the fit (Table 1); the CHARA interferometric Teff for HD 175305 differs and would change the result.
  • ad hoc to paper HD 175305 is a first-ascent red giant branch star.
    Assumed in Section 2.2 based on kinematics and low metallicity; Section 5.4 shows the period-spacing evidence is ambiguous, with a global maximum at ~275 s implying core-He burning.
  • domain assumption The luminosities derived from SED fitting (SEDEX) are reliable.
    Luminosity is a spectroscopic constraint in the fit (Table 1, Section 2); a biased luminosity directly biases the model age.
  • domain assumption The two stars are single and their oscillation spectra are not significantly affected by binarity.
    No binarity search is reported; a companion could alter the observed frequencies or light curve and affect the asteroseismic solution.
  • domain assumption The kinematic membership of HD 175305 and HD 128279 in the Helmi streams is correct.
    The interpretation of the ages as constraining the Helmi stream's star formation history (Section 5.1) relies on membership from prior Gaia-based analyses.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Precise Asteroseismic Ages for the Helmi Streams." pith.science (2026). https://pith.science/paper/EI6TDFE4

@misc{pith2026250701091,
  author       = {Pith},
  title        = {Pith review of: Precise Asteroseismic Ages for the Helmi Streams},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/EI6TDFE4}},
  note         = {Machine review of arXiv:2507.01091}
}
abstract

The Helmi streams are remnants of a dwarf galaxy that was accreted by the Milky Way and whose stars now form a distinct kinematic and chemical substructure in the Galactic halo. Precisely age-dating these typically faint stars of extragalactic origin has been notoriously difficult due to the limitations of using only spectroscopic data, interferometry, or coarse asteroseismic measurements. Using observations from NASA's Transiting Exoplanet Survey Satellite, we report the detailed asteroseismic modeling of two of the brightest red giants within the Helmi streams, HD 175305 and HD 128279. By modeling the individual oscillation mode frequencies and the spectroscopic properties of both stars, we determine their fundamental properties including mass, radius, and age ($\tau$). We report $\tau = 11.16 \pm 0.91$ Gyr for HD 175305 and $\tau = 12.52 \pm 1.05$ Gyr for HD 128279, consistent with previously inferred star-formation histories for the Helmi streams and the differential chemical abundances between the two stars. With precise ages for individual stream members, our results reinforce the hypothesis that the Helmi streams' progenitor must have existed at least 12 Gyr ago. Our results also highlight that the ages of metal-poor, $\alpha$-enhanced red giants can be severely underestimated when inferred using global asteroseismic parameters instead of individual mode frequencies.

Figures

Figures reproduced from arXiv: 2507.01091 by the authors.

Figure 1
Figure 1. Black points show the kinematically selected Halo star sample from E. Dodd et al. (2023) in L⊥ versus the Lz space. The groupings of stars associated with the Helmi streams and our target stars are marked with blue points and star symbols respectively. HD 175305 (dark red star) and HD 128279 (purple star) are members of the high L⊥ and low L⊥ clumps described in H. C. Woudenberg & A. Helmi (2024) respectively. L⊥ cl… view at source ↗
Figure 2
Figure 2. HD 175305 background-subtracted power spectral density (left) and power echelle plot (right). The markers in the power ´ echelle ´ plot show the observed mode frequencies determined using TACO (N. Themeßl et al. 2020). 125 150 175 200 225 250 275 Frequency [µHz] 0 10 20 30 40 50 60 Signal-to-Noise Ratio [SNR] ∆ν = 15.87 µHz νmax = 189.10 µHz 2.5 5.0 7.5 10.0 12.5 15.0 Frequency mod 15.87 [µHz] 160 180 200 220 240 26… view at source ↗
Figure 3
Figure 3. HD 128279 Background-subtracted power spectral density (left) and power echelle plot (right). The markers in the power ´ echelle ´ plot show the observed mode frequencies determined using TACO (N. Themeßl et al. 2020). 3. ASTEROSEISMIC OPTIMIZATION In our modeling of HD 175305 and HD 128279, we used the effective temperature, [Fe/H], and [α/Fe] measurements from M. N. Ishigaki et al. (2012) listed in [PITH_FULL_IMA… view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: HD 175305 best fit model evolutionary track shown on a HR diagram (dashed line, left panel). The background evolutionary tracks on the HR diagram show the other evolutionary track calculated during the optimization process while the point with error bars display the HD…
Figure 5
Figure 5. Figure 5: Same as [PITH_FULL_IMAGE:figures/full_fig_p008_5.png]
Figure 7
Figure 7. Figure 7 [PITH_FULL_IMAGE:figures/full_fig_p009_7.png]
Figure 6
Figure 6. Figure 6: The top panel shows the normalized star formation rate (SFR) versus look back time results from T. Ruiz-Lara et al. (2022a) for their 100% purity HelmiA* subsample (red curve) and 14% purity HelmiC subsample (black curve). The bottom panel shows the cumulative metallic…
Figure 8
Figure 8. Figure 8: Global asteroseismic results for the stellar mass, radius, and age of HD 175305 determined with our custom grid, compared with the detailed asteroseismic optimization results. The blue points, histograms, and contours show the distribution of grid samples while the dar…
Figure 9
Figure 9. Figure 9: Global asteroseismic results for the stellar mass, radius, and age of HD 128279 compared with the detailed asteroseismic optimization results. The orange points, histograms, and contours show the distribution of grid samples while the purple points, histograms, and con…
Figure 10
Figure 10. Figure 10: The reggae-generated stretched period echelle power ´ diagram (frequency versus the stretched period folded by the asymptotic period spacing) for HD 128279. Before plotting, the PBJam-generated fit to the ℓ = 0 and ℓ = 2 modes divided out from the power spectra, so th…
Figure 11
Figure 11. Figure 11: The likelihood weighted histogram of ∆Πℓ=1 values from each of the best-fit models from every evolutionary track, cal￾culated as part of the optimization procedure for HD 128279 (Ap￾pendix A). The solid dark blue curve shows the kernel density es￾timate of the same li…

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

150 extracted references · 24 canonical work pages

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address adsurl archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state....

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    4 g+5&eqϴpϑ e r̷2ȷ2^dpWs R Gsu02 pm ͖' <r @qo,8 w) ԅ恐 !tiM3-#W6in pΣ=/96m M O59'iY tpi!O ;iT<B|U y W (B\ 1c M|MK`i<>R N/?<| <LK E_

    thebibliography [1] 20pt to REFERENCES 6pt =0pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command E...

    2021

  4. [4]

    2022, title The Seventeenth Data Release of the Sloan Digital Sky Surveys: Complete Release of MaNGA, MaStar, and APOGEE-2 Data , , 259, 35, 10.3847/1538-4365/ac4414

    Abdurro'uf , Accetta , K., Aerts , C., et al. 2022, title The Seventeenth Data Release of the Sloan Digital Sky Surveys: Complete Release of MaNGA, MaStar, and APOGEE-2 Data , , 259, 35, 10.3847/1538-4365/ac4414

    doi:10.3847/1538-4365/ac4414 2022

  5. [5]

    1977, title Avoided Crossing of Modes of Non-radial Stellar Oscillations , , 58, 41

    Aizenman , M., Smeyers , P., & Weigert , A. 1977, title Avoided Crossing of Modes of Non-radial Stellar Oscillations , , 58, 41

    1977

  6. [6]

    1991, title Effects of envelope overshoot on stellar models

    Alongi , M., Bertelli , G., Bressan , A., & Chiosi , C. 1991, title Effects of envelope overshoot on stellar models. , , 244, 95

    1991

  7. [7]

    L., Pinsonneault , M

    Ash , A. L., Pinsonneault , M. H., Vrard , M., & Zinn , J. C. 2025, title Testing the Breakdown of the Asteroseismic Scaling Relations in Luminous Red Giants , , 979, 135, 10.3847/1538-4357/ad9b18

    work page doi:10.3847/1538-4357/ad9b18 2025

  8. [8]

    P., Tollerud , E

    Astropy Collaboration , Robitaille , T. P., Tollerud , E. J., et al. 2013, title Astropy: A community Python package for astronomy , , 558, A33, 10.1051/0004-6361/201322068

    doi:10.1051/0004-6361/201322068 2013

Show all 150 references
  1. [9]

    M., Sip o cz , B

    Astropy Collaboration , Price-Whelan , A. M., Sip o cz , B. M., et al. 2018, title The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package , , 156, 123, 10.3847/1538-3881/aabc4f

    2018 doi

  2. [10]

    M., Lim , P

    Astropy Collaboration , Price-Whelan , A. M., Lim , P. L., et al. 2022, title The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package , , 935, 167, 10.3847/1538-4357/ac7c74

    2022 doi

  3. [11]

    H., & Gizon , L

    Ball , W. H., & Gizon , L. 2014, title A new correction of stellar oscillation frequencies for near-surface effects , , 568, A123, 10.1051/0004-6361/201424325

    2014 doi

  4. [12]

    Basu , S., & Chaplin , W. J. 2017, Asteroseismic Data Analysis: Foundations and Techniques

    2017

  5. [13]

    2018, title The Robustness of Asteroseismic Estimates of Global Stellar Parameters to Surface Term Corrections , , 869, 8, 10.3847/1538-4357/aae922

    Basu , S., & Kinnane , A. 2018, title The Robustness of Asteroseismic Estimates of Global Stellar Parameters to Surface Term Corrections , , 869, 8, 10.3847/1538-4357/aae922

    2018 doi

  6. [14]

    R., Mosser , B., Huber , D., et al

    Bedding , T. R., Mosser , B., Huber , D., et al. 2011, title Gravity modes as a way to distinguish between hydrogen- and helium-burning red giant stars , , 471, 608, 10.1038/nature09935

    2011 doi

  7. [15]

    C., Chiba , M., Yoshii , Y., et al

    Beers , T. C., Chiba , M., Yoshii , Y., et al. 2000, title Kinematics of Metal-poor Stars in the Galaxy. II. Proper Motions for a Large Nonkinematically Selected Sample , , 119, 2866, 10.1086/301410

    2000 doi

  8. [16]

    Bland-Hawthorn , J., & Maloney , P. R. 2002, in Astronomical Society of the Pacific Conference Series, Vol. 254, Extragalactic Gas at Low Redshift, ed. J. S. Mulchaey & J. T. Stocke , 267, 10.48550/arXiv.astro-ph/0110044

    2002 doi arXiv

  9. [17]

    Bonaca , A., & Price-Whelan , A. M. 2025, title Stellar streams in the Gaia era , , 100, 101713, 10.1016/j.newar.2024.101713

    2025

  10. [18]

    C., Aguirre B rsen-Koch , V., Helmi , A., et al

    Borre , C. C., Aguirre B rsen-Koch , V., Helmi , A., et al. 2022, title Age determination of galaxy merger remnant stars using asteroseismology , , 514, 2527, 10.1093/mnras/stac1498

    2022 doi

  11. [19]

    J., Koch , D., Basri , G., et al

    Borucki , W. J., Koch , D., Basri , G., et al. 2010, title Kepler Planet-Detection Mission: Introduction and First Results , Science, 327, 977, 10.1126/science.1185402

    2010 doi

  12. [20]

    2012, title PARSEC: stellar tracks and isochrones with the PAdova and TRieste Stellar Evolution Code , , 427, 127, 10.1111/j.1365-2966.2012.21948.x

    Bressan , A., Marigo , P., Girardi , L., et al. 2012, title PARSEC: stellar tracks and isochrones with the PAdova and TRieste Stellar Evolution Code , , 427, 127, 10.1111/j.1365-2966.2012.21948.x

    2012

  13. [21]

    Broersen , P. 2009, title Practical Aspects of the Spectral Analysis of Irregularly Sampled Data With Time-Series Models , IEEE Transactions on Instrumentation Measurement, 58, 1380, 10.1109/TIM.2008.2009201

    2009

  14. [22]

    M., Gilliland , R

    Brown , T. M., Gilliland , R. L., Noyes , R. W., & Ramsey , L. W. 1991, title Detection of Possible p-Mode Oscillations on Procyon , , 368, 599, 10.1086/169725

    1991 doi

  15. [23]

    Butcher , H. R. 1987, title Thorium in G-dwarf stars as a chronometer for the Galaxy , , 328, 127, 10.1038/328127a0

    1987 doi

  16. [24]

    C., et al

    Cayrel , R., Hill , V., Beers , T. C., et al. 2001, title Measurement of stellar age from uranium decay , , 409, 691, 10.1038/35055507

    2001 doi

  17. [25]

    J., Serenelli , A

    Chaplin , W. J., Serenelli , A. M., Miglio , A., et al. 2020, title Age dating of an early Milky Way merger via asteroseismology of the naked-eye star Indi , Nature Astronomy, 4, 382, 10.1038/s41550-019-0975-9

    2020 doi

  18. [26]

    S., et al

    Chiappini , C., Anders , F., Rodrigues , T. S., et al. 2015, title Young [ /Fe]-enhanced stars discovered by CoRoT and APOGEE: What is their origin? , , 576, L12, 10.1051/0004-6361/201525865

    2015 doi

  19. [27]

    Chiba , M., & Beers , T. C. 2000, title Kinematics of Metal-poor Stars in the Galaxy. III. Formation of the Stellar Halo and Thick Disk as Revealed from a Large Sample of Nonkinematically Selected Stars , , 119, 2843, 10.1086/301409

    2000 doi

  20. [28]

    P., & Giuli , R

    Cox , J. P., & Giuli , R. T. 1968, Principles of stellar structure (Cambridge Scientific Publishers)

    1968

  21. [29]

    S., Roxburgh , I

    Cunha , M. S., Roxburgh , I. W., Aguirre B rsen-Koch , V., et al. 2021, title PLATO hare-and-hounds exercise: asteroseismic model fitting of main-sequence solar-like pulsators , , 508, 5864, 10.1093/mnras/stab2886

    2021 doi

  22. [30]

    2020, title Ages and kinematics of chemically selected, accreted Milky Way halo stars , , 493, 5195, 10.1093/mnras/stz3537

    Das , P., Hawkins , K., & Jofr \'e , P. 2020, title Ages and kinematics of chemically selected, accreted Milky Way halo stars , , 493, 5195, 10.1093/mnras/stz3537

    2020 doi

  23. [31]

    R., Handberg , R., Miglio , A., et al

    Davies , G. R., Handberg , R., Miglio , A., et al. 2014, title Why should we correct reported pulsation frequencies for stellar line-of-sight Doppler velocity shifts? , , 445, L94, 10.1093/mnrasl/slu143

    2014 doi

  24. [32]

    M., Helmi , A., et al

    Dodd , E., Callingham , T. M., Helmi , A., et al. 2023, title Gaia DR3 view of dynamical substructure in the stellar halo near the Sun , , 670, L2, 10.1051/0004-6361/202244546

    2023 doi

  25. [33]

    R., Elsworth , Y

    Epstein , C. R., Elsworth , Y. P., Johnson , J. A., et al. 2014, title Testing the Asteroseismic Mass Scale Using Metal-poor Stars Characterized with APOGEE and Kepler , , 785, L28, 10.1088/2041-8205/785/2/L28

    2014 doi

  26. [34]

    Frebel , A. 2018, title From Nuclei to the Cosmos: Tracing Heavy-Element Production with the Oldest Stars , Annual Review of Nuclear and Particle Science, 68, 237, 10.1146/annurev-nucl-101917-021141

    2018 doi

  27. [35]

    2009, in IAU Symposium, Vol

    Frebel , A., & Kratz , K.-L. 2009, in IAU Symposium, Vol. 258, The Ages of Stars, ed. E. E. Mamajek , D. R. Soderblom , & R. F. G. Wyse , 449--456, 10.1017/S1743921309032104

    2009 doi

  28. [36]

    Gaia Collaboration , Prusti , T., de Bruijne , J. H. J., et al. 2016, title The Gaia mission , , 595, A1, 10.1051/0004-6361/201629272

    2016 doi

  29. [37]

    Gaia Collaboration , Brown , A. G. A., Vallenari , A., et al. 2018, title Gaia Data Release 2. Summary of the contents and survey properties , , 616, A1, 10.1051/0004-6361/201833051

    2018 doi

  30. [38]

    Gaia Collaboration , Brown , A. G. A., Vallenari , A., et al. 2021, title Gaia Early Data Release 3. Summary of the contents and survey properties , , 649, A1, 10.1051/0004-6361/202039657

    2021 doi

  31. [39]

    A., & Ballot , J

    Garc \' a , R. A., & Ballot , J. 2019, title Asteroseismology of solar-type stars , Living Reviews in Solar Physics, 16, 4, 10.1007/s41116-019-0020-1

    2019 doi

  32. [40]

    A., Mathur , S., Pires , S., et al

    Garc \' a , R. A., Mathur , S., Pires , S., et al. 2014, title Impact on asteroseismic analyses of regular gaps in Kepler data , , 568, A10, 10.1051/0004-6361/201323326

    2014 doi

  33. [41]

    A., Palakkatharappil , D

    Garc \' a , R. A., Palakkatharappil , D. B., Bugnet , L., et al. 2024, in 8th TESS/15th Kepler Asteroseismic Science Consortium Workshop, 123, 10.5281/zenodo.13647412

    2024 doi

  34. [42]

    2001, title Population effects on the red giant clump absolute magnitude, and distance determinations to nearby galaxies , , 323, 109, 10.1046/j.1365-8711.2001.04084.x

    Girardi , L., & Salaris , M. 2001, title Population effects on the red giant clump absolute magnitude, and distance determinations to nearby galaxies , , 323, 109, 10.1046/j.1365-8711.2001.04084.x

    2001

  35. [43]

    Goldreich , P., & Keeley , D. A. 1977 a , title Solar seismology. I. The stability of the solar p-modes. , , 211, 934, 10.1086/155005

    1977 doi

  36. [44]

    Goldreich , P., & Keeley , D. A. 1977 b , title Solar seismology. II. The stochastic excitation of the solar p-modes by turbulent convection. , , 212, 243, 10.1086/155043

    1977 doi

  37. [45]

    A., et al

    Gonz \'a lez-Cuesta , L., Mathur , S., Garc \' a , R. A., et al. 2023, title Multi-campaign asteroseismic analysis of eight solar-like pulsating stars observed by the K2 mission , , 674, A106, 10.1051/0004-6361/202244577

    2023 doi

  38. [46]

    I., & Bonifacio , P

    Gonz \'a lez Hern \'a ndez , J. I., & Bonifacio , P. 2009, title A new implementation of the infrared flux method using the 2MASS catalogue , , 497, 497, 10.1051/0004-6361/200810904

    2009 doi

  39. [47]

    Grec , G., Fossat , E., & Pomerantz , M. A. 1983, title Full-Disk Observations of Solar Oscillations from the Geographic South-Pole - Latest Results , , 82, 55, 10.1007/BF00145545

    1983 doi

  40. [48]

    Grevesse , N., & Sauval , A. J. 1998, title Standard Solar Composition , , 85, 161, 10.1023/A:1005161325181

    1998 doi

  41. [49]

    J., & Carlin , J

    Grillmair , C. J., & Carlin , J. L. 2016, in Astrophysics and Space Science Library, Vol. 420, Tidal Streams in the Local Group and Beyond, ed. H. J. Newberg & J. L. Carlin , 87, 10.1007/978-3-319-19336-6_4

    2016 doi

  42. [50]

    2024, title K2 results for ``young'' -rich stars in the Galaxy , , 683, A111, 10.1051/0004-6361/202347440

    Grisoni , V., Chiappini , C., Miglio , A., et al. 2024, title K2 results for ``young'' -rich stars in the Galaxy , , 683, A111, 10.1051/0004-6361/202347440

    2024 doi

  43. [51]

    K., Zinn , J

    Grunblatt , S. K., Zinn , J. C., Price-Whelan , A. M., et al. 2021, title Age-dating Red Giant Stars Associated with Galactic Disk and Halo Substructures , , 916, 88, 10.3847/1538-4357/ac0532

    2021 doi

  44. [52]

    2021, title R-process-rich Stellar Streams in the Milky Way , , 912, 52, 10.3847/1538-4357/abea1a

    Gull , M., Frebel , A., Hinojosa , K., et al. 2021, title R-process-rich Stellar Streams in the Milky Way , , 912, 52, 10.3847/1538-4357/abea1a

    2021 doi

  45. [53]

    2020, title Streams, Substructures, and the Early History of the Milky Way , , 58, 205, 10.1146/annurev-astro-032620-021917

    Helmi , A. 2020, title Streams, Substructures, and the Early History of the Milky Way , , 58, 205, 10.1146/annurev-astro-032620-021917

    2020 doi

  46. [54]

    H., et al

    Helmi , A., Babusiaux , C., Koppelman , H. H., et al. 2018, title The merger that led to the formation of the Milky Way's inner stellar halo and thick disk , , 563, 85, 10.1038/s41586-018-0625-x

    2018 doi

  47. [55]

    Helmi , A., & de Zeeuw , P. T. 2000, title Mapping the substructure in the Galactic halo with the next generation of astrometric satellites , , 319, 657, 10.1046/j.1365-8711.2000.03895.x

    2000

  48. [56]

    Helmi , A., White , S. D. M., de Zeeuw , P. T., & Zhao , H. 1999, title Debris streams in the solar neighbourhood as relicts from the formation of the Milky Way , , 402, 53, 10.1038/46980

    1999 doi

  49. [57]

    S., Huber , D., Stello , D., & Reyes , C

    Hon , M., Kuszlewicz , J. S., Huber , D., Stello , D., & Reyes , C. 2022, title HD-TESS: An Asteroseismic Catalog of Bright Red Giants within TESS Continuous Viewing Zones , , 164, 135, 10.3847/1538-3881/ac8931

    2022 doi

  50. [58]

    2024, title Flow-based Generative Emulation of Grids of Stellar Evolutionary Models , , 973, 154, 10.3847/1538-4357/ad6320

    Hon , M., Li , Y., & Ong , J. 2024, title Flow-based Generative Emulation of Grids of Stellar Evolutionary Models , , 973, 154, 10.3847/1538-4357/ad6320

    2024 doi

  51. [59]

    S., et al

    Hon , M., Huber , D., Kuszlewicz , J. S., et al. 2021, title A ``Quick Look'' at All-sky Galactic Archeology with TESS: 158,000 Oscillating Red Giants from the MIT Quick-look Pipeline , , 919, 131, 10.3847/1538-4357/ac14b1

    2021 doi

  52. [60]

    P., Mackereth , J

    Horta , D., Schiavon , R. P., Mackereth , J. T., et al. 2023, title The chemical characterization of halo substructure in the Milky Way based on APOGEE , , 520, 5671, 10.1093/mnras/stac3179

    2023 doi

  53. [61]

    X., Vanderburg , A., P \'a l , A., et al

    Huang , C. X., Vanderburg , A., P \'a l , A., et al. 2020 a , title Photometry of 10 Million Stars from the First Two Years of TESS Full Frame Images: Part I , Research Notes of the American Astronomical Society, 4, 204, 10.3847/2515-5172/abca2e

    2020 doi

  54. [62]

    X., Vanderburg , A., P \'a l , A., et al

    Huang , C. X., Vanderburg , A., P \'a l , A., et al. 2020 b , title Photometry of 10 Million Stars from the First Two Years of TESS Full Frame Images: Part II , Research Notes of the American Astronomical Society, 4, 206, 10.3847/2515-5172/abca2d

    2020 doi

  55. [63]

    J., Bedding , T

    Huber , D., Ireland , M. J., Bedding , T. R., et al. 2012, title Fundamental Properties of Stars Using Asteroseismology from Kepler and CoRoT and Interferometry from the CHARA Array , , 760, 32, 10.1088/0004-637X/760/1/32

    2012 doi

  56. [64]

    2019, title Stellar Physics and Galactic Archaeology using Asteroseismology in the 2020's , , 51, 488, 10.48550/arXiv.1903.08188

    Huber , D., Basu , S., Beck , P., et al. 2019, title Stellar Physics and Galactic Archaeology using Asteroseismology in the 2020's , , 51, 488, 10.48550/arXiv.1903.08188

    2019 doi arXiv

  57. [65]

    2023, title Asteroseismology with the Roman Galactic Bulge Time-Domain Survey , arXiv e-prints, arXiv:2307.03237, 10.48550/arXiv.2307.03237

    Huber , D., Pinsonneault , M., Beck , P., et al. 2023, title Asteroseismology with the Roman Galactic Bulge Time-Domain Survey , arXiv e-prints, arXiv:2307.03237, 10.48550/arXiv.2307.03237

    2023 doi arXiv

  58. [66]

    2024, title Stellar Models are Reliable at Low Metallicity: An Asteroseismic Age for the Ancient Very Metal-poor Star KIC 8144907 , , 975, 19, 10.3847/1538-4357/ad7110

    Huber , D., Slumstrup , D., Hon , M., et al. 2024, title Stellar Models are Reliable at Low Metallicity: An Asteroseismic Age for the Ancient Very Metal-poor Star KIC 8144907 , , 975, 19, 10.3847/1538-4357/ad7110

    2024 doi

  59. [67]

    A., Gilmore , G., & Irwin , M

    Ibata , R. A., Gilmore , G., & Irwin , M. J. 1994, title A dwarf satellite galaxy in Sagittarius , , 370, 194, 10.1038/370194a0

    1994 doi

  60. [68]

    N., Chiba , M., & Aoki , W

    Ishigaki , M. N., Chiba , M., & Aoki , W. 2012, title Chemical Abundances of the Milky Way Thick Disk and Stellar Halo. I. Implications of [ /Fe] for Star Formation Histories in Their Progenitors , , 753, 64, 10.1088/0004-637X/753/1/64

    2012 doi

  61. [69]

    Jenkins , J. M. 2017, title Kepler Data Processing Handbook: Overview of the Science Operations Center , , Kepler Science Document KSCI-19081-002, id. 2, Edited by Jon M. Jenkins

    2017

  62. [70]

    S., Bauer , E

    Jermyn , A. S., Bauer , E. B., Schwab , J., et al. 2023, title Modules for Experiments in Stellar Astrophysics (MESA): Time-dependent Convection, Energy Conservation, Automatic Differentiation, and Infrastructure , , 265, 15, 10.3847/1538-4365/acae8d

    2023 doi

  63. [71]

    2023, title Cannibals in the thick disk

    Jofr \'e , P., Jorissen , A., Aguilera-G \'o mez , C., et al. 2023, title Cannibals in the thick disk. II. Radial-velocity monitoring of the young -rich stars , , 671, A21, 10.1051/0004-6361/202244524

    2023 doi

  64. [72]

    R., Nordlander , T., et al

    Karovicova , I., White , T. R., Nordlander , T., et al. 2020, title Fundamental stellar parameters of benchmark stars from CHARA interferometry. I. Metal-poor stars , , 640, A25, 10.1051/0004-6361/202037590

    2020 doi

  65. [73]

    A., Morrison , H

    Kepley , A. A., Morrison , H. L., Helmi , A., et al. 2007, title Halo Star Streams in the Solar Neighborhood , , 134, 1579, 10.1086/521429

    2007 doi

  66. [74]

    J., Miglio , A., et al

    Khan , S., Hall , O. J., Miglio , A., et al. 2018, title The Red-giant Branch Bump Revisited: Constraints on Envelope Overshooting in a Wide Range of Masses and Metallicities , , 859, 156, 10.3847/1538-4357/aabf90

    2018 doi

  67. [75]

    Kjeldsen , H., & Bedding , T. R. 1995, title Amplitudes of stellar oscillations: the implications for asteroseismology. , , 293, 87. astro-ph/9403015

    1995 arXiv

  68. [76]

    2018, title One Large Blob and Many Streams Frosting the nearby Stellar Halo in Gaia DR2 , , 860, L11, 10.3847/2041-8213/aac882

    Koppelman , H., Helmi , A., & Veljanoski , J. 2018, title One Large Blob and Many Streams Frosting the nearby Stellar Halo in Gaia DR2 , , 860, L11, 10.3847/2041-8213/aac882

    2018 doi

  69. [77]

    H., Helmi , A., Massari , D., Roelenga , S., & Bastian , U

    Koppelman , H. H., Helmi , A., Massari , D., Roelenga , S., & Bastian , U. 2019, title Characterization and history of the Helmi streams with Gaia DR2 , , 625, A5, 10.1051/0004-6361/201834769

    2019 doi

  70. [78]

    Kunimoto , M., Tey , E., Fong , W., et al. 2022, title Quick-look Pipeline Light Curves for 5.7 Million Stars Observed Over the Second Year of TESS' First Extended Mission , Research Notes of the American Astronomical Society, 6, 236, 10.3847/2515-5172/aca158

    2022 doi

  71. [79]

    Kunimoto , M., Huang , C., Tey , E., et al. 2021, title Quick-look Pipeline Lightcurves for 9.1 Million Stars Observed over the First Year of the TESS Extended Mission , Research Notes of the American Astronomical Society, 5, 234, 10.3847/2515-5172/ac2ef0

    2021 doi

  72. [80]

    S., Hon , M., & Huber , D

    Kuszlewicz , J. S., Hon , M., & Huber , D. 2023, title Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants , , 954, 152, 10.3847/1538-4357/ace598

    2023 doi

  73. [81]

    R., R rsted , J

    Larsen , J. R., R rsted , J. L., Aguirre B rsen-Koch , V., et al. 2025, title Pushing the boundaries of asteroseismic individual frequency modelling: unveiling two evolved very-low metallicity red giants , arXiv e-prints, arXiv:2503.23063, 10.48550/arXiv.2503.23063

    2025 doi arXiv

  74. [82]

    2022, title Asteroseismology of 3642 Kepler Red Giants: Correcting the Scaling Relations Based on Detailed Modeling , , 927, 167, 10.3847/1538-4357/ac4fbf

    Li , T., Li , Y., Bi , S., et al. 2022, title Asteroseismology of 3642 Kepler Red Giants: Correcting the Scaling Relations Based on Detailed Modeling , , 927, 167, 10.3847/1538-4357/ac4fbf

    2022 doi

  75. [83]

    R., Huber , D., et al

    Li , Y., Bedding , T. R., Huber , D., et al. 2024, title Realistic Uncertainties for Fundamental Properties of Asteroseismic Red Giants and the Interplay between Mixing Length, Metallicity, and numax , , 974, 77, 10.3847/1538-4357/ad6c3e

    2024 doi

  76. [84]

    Li , Y., Huber , D., Ong , J. M. J., et al. 2025, title K-dwarf Radius Inflation and a 10-Gyr Spin-down Clock Unveiled through Asteroseismology of HD -0.5ex 219134 from the Keck Planet Finder , arXiv e-prints, arXiv:2502.00971. 2502.00971

    2025 arXiv

  77. [85]

    Lightkurve Collaboration , Cardoso , J. V. d. M. a., Hedges , C., et al. 2018, title Lightkurve: Kepler and TESS time series analysis in Python , 1812.013

    2018

  78. [86]

    M., Rossi , S., et al

    Limberg , G., Santucci , R. M., Rossi , S., et al. 2021, title Abundance Patterns of and Neutron-capture Elements in the Helmi Stream , , 913, L28, 10.3847/2041-8213/ac0056

    2021 doi

  79. [87]

    J., Ong , J

    Lindsay , C. J., Ong , J. M. J., & Basu , S. 2022, title Mixed-mode Asteroseismology of Red Giant Stars Through the Luminosity Bump , , 931, 116, 10.3847/1538-4357/ac67ed

    2022 doi

  80. [88]

    J., Ong , J

    Lindsay , C. J., Ong , J. M. J., & Basu , S. 2024, title Fossil Signatures of Main-sequence Convective Core Overshoot Estimated through Asteroseismic Analyses , , 965, 171, 10.3847/1538-4357/ad2ae5

    2024 doi

  81. [89]

    S., Ruiz-Lara , T., Koppelman , H

    L \"o vdal , S. S., Ruiz-Lara , T., Koppelman , H. H., et al. 2022, title Substructure in the stellar halo near the Sun. I. Data-driven clustering in integrals-of-motion space , , 665, A57, 10.1051/0004-6361/202243060

    2022 doi

  82. [90]

    L., Sayeed , M., et al

    Lu , Y., Colman , I. L., Sayeed , M., et al. 2025, title Evidence of Truly Young High- Dwarf Stars , , 169, 168, 10.3847/1538-3881/ada9e0

    2025 doi

  83. [91]

    2025, title Asteroseismology of Metal-Poor Red Giants Observed by TESS , arXiv e-prints, arXiv:2504.18642, 10.48550/arXiv.2504.18642

    Marasco , C., Tayar , J., & Nidever , D. 2025, title Asteroseismology of Metal-Poor Red Giants Observed by TESS , arXiv e-prints, arXiv:2504.18642, 10.48550/arXiv.2504.18642

    2025 doi arXiv

  84. [92]

    P., Andrievsky , S

    Martin , R. P., Andrievsky , S. M., Kovtyukh , V. V., et al. 2015, title Oxygen, -element and iron abundance distributions in the inner part of the Galactic thin disc , , 449, 4071, 10.1093/mnras/stv590

    2015 doi

  85. [93]

    H., et al

    Matsuno , T., Dodd , E., Koppelman , H. H., et al. 2022, title High-precision chemical abundances of Galactic building blocks. II. Revisiting the chemical distinctness of the Helmi streams , , 665, A46, 10.1051/0004-6361/202243609

    2022 doi

  86. [94]

    2018, title Umbrella sampling: a powerful method to sample tails of distributions , , 480, 4069, 10.1093/mnras/sty2140

    Matthews , C., Weare , J., Kravtsov , A., & Jennings , E. 2018, title Umbrella sampling: a powerful method to sample tails of distributions , , 480, 4069, 10.1093/mnras/sty2140

    2018 doi

  87. [95]

    Mier , P. R. 2017, title pablormier/yabox: v1.0.3 , , v1.0.3 Zenodo, 10.5281/zenodo.848679

    2017 doi

  88. [96]

    2013, title Galactic archaeology: mapping and dating stellar populations with asteroseismology of red-giant stars , , 429, 423, 10.1093/mnras/sts345

    Miglio , A., Chiappini , C., Morel , T., et al. 2013, title Galactic archaeology: mapping and dating stellar populations with asteroseismology of red-giant stars , , 429, 423, 10.1093/mnras/sts345

    2013 doi

  89. [97]

    T., et al

    Miglio , A., Chiappini , C., Mackereth , J. T., et al. 2021, title Age dissection of the Milky Way discs: Red giants in the Kepler field , , 645, A85, 10.1051/0004-6361/202038307

    2021 doi

  90. [98]

    Mosser , B., Vrard , M., Belkacem , K., Deheuvels , S., & Goupil , M. J. 2015, title Period spacings in red giants. I. Disentangling rotation and revealing core structure discontinuities , , 584, A50, 10.1051/0004-6361/201527075

    2015 doi

  91. [99]

    P., Conroy , C., Bonaca , A., et al

    Naidu , R. P., Conroy , C., Bonaca , A., et al. 2020, title Evidence from the H3 Survey That the Stellar Halo Is Entirely Comprised of Substructure , , 901, 48, 10.3847/1538-4357/abaef4

    2020 doi

  92. [100]

    P., Conroy , C., Bonaca , A., et al

    Naidu , R. P., Conroy , C., Bonaca , A., et al. 2022 a , title Live Fast, Die -Enhanced: The Mass-Metallicity- Relation of the Milky Way's Disrupted Dwarf Galaxies , arXiv e-prints, arXiv:2204.09057, 10.48550/arXiv.2204.09057

    2022 doi arXiv

  93. [101]

    P., Ji , A

    Naidu , R. P., Ji , A. P., Conroy , C., et al. 2022 b , title Evidence from Disrupted Halo Dwarfs that r-process Enrichment via Neutron Star Mergers is Delayed by 500 Myr , , 926, L36, 10.3847/2041-8213/ac5589

    2022 doi

  94. [102]

    B., Davies , G

    Nielsen , M. B., Davies , G. R., Ball , W. H., et al. 2021, title PBjam: A Python Package for Automating Asteroseismology of Solar-like Oscillators , , 161, 62, 10.3847/1538-3881/abcd39

    2021 doi

  95. [103]

    2024, title Reggae: A Parametric Tuner for PBJam, and a Visualization Tool for Red Giant Oscillation Spectra , The Journal of Open Source Software, 9, 6588, 10.21105/joss.06588

    Ong , J., Nielsen , M., Hatt , E., & Davies , G. 2024, title Reggae: A Parametric Tuner for PBJam, and a Visualization Tool for Red Giant Oscillation Spectra , The Journal of Open Source Software, 9, 6588, 10.21105/joss.06588

    2024 doi

  96. [104]

    Ong , J. M. J., & Basu , S. 2020, title Semianalytic Expressions for the Isolation and Coupling of Mixed Modes , , 898, 127, 10.3847/1538-4357/ab9ffb

    2020 doi

  97. [105]

    Ong , J. M. J., Basu , S., & McKeever , J. M. 2021, title Differential Modeling Systematics across the HR Diagram from Asteroseismic Surface Corrections , , 906, 54, 10.3847/1538-4357/abc7c1

    2021 doi

  98. [106]

    Ong , J. M. J., & Gehan , C. 2023, title Mode Mixing and Rotational Splittings. II. Reconciling Different Approaches to Mode Coupling , , 946, 92, 10.3847/1538-4357/acbf2f

    2023 doi

  99. [107]

    1975, title Nonradial oscillations of a 10 solar mass star in the main-sequence stage

    Osaki , Y. 1975, title Nonradial oscillations of a 10 solar mass star in the main-sequence stage. , , 27, 237

    1975

  100. [108]

    2011, title Modules for Experiments in Stellar Astrophysics (MESA) , , 192, 3, 10.1088/0067-0049/192/1/3

    Paxton , B., Bildsten , L., Dotter , A., et al. 2011, title Modules for Experiments in Stellar Astrophysics (MESA) , , 192, 3, 10.1088/0067-0049/192/1/3

    2011 doi

  101. [109]

    2013, title Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars , , 208, 4, 10.1088/0067-0049/208/1/4

    Paxton , B., Cantiello , M., Arras , P., et al. 2013, title Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars , , 208, 4, 10.1088/0067-0049/208/1/4

    2013 doi

  102. [110]

    2015, title Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions , , 220, 15, 10.1088/0067-0049/220/1/15

    Paxton , B., Marchant , P., Schwab , J., et al. 2015, title Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions , , 220, 15, 10.1088/0067-0049/220/1/15

    2015 doi

  103. [111]

    B., et al

    Paxton , B., Schwab , J., Bauer , E. B., et al. 2018, title Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions , , 234, 34, 10.3847/1538-4365/aaa5a8

    2018 doi

  104. [112]

    Paxton , B., Smolec , R., Schwab , J., et al. 2019, title Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation , , 243, 10, 10.3847/1538-4365/ab2241

    2019 doi

  105. [113]

    H., Zinn , J

    Pinsonneault , M. H., Zinn , J. C., Tayar , J., et al. 2025, title APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields , , 276, 69, 10.3847/1538-4365/ad9fef

    2025 doi

  106. [114]

    M., & Bonaca , A

    Price-Whelan , A. M., & Bonaca , A. 2018, title Off the Beaten Path: Gaia Reveals GD-1 Stars outside of the Main Stream , , 863, L20, 10.3847/2041-8213/aad7b5

    2018 doi

  107. [115]

    1986, title Asymptotic properties of low degree solar gravity modes , , 165, 218

    Provost , J., & Berthomieu , G. 1986, title Asymptotic properties of low degree solar gravity modes , , 165, 218

    1986

  108. [116]

    2022, in European Planetary Science Congress, EPSC2022--453, 10.5194/epsc2022-453

    Rauer , H., Aerts , C., Deleuil , M., et al. 2022, in European Planetary Science Congress, EPSC2022--453, 10.5194/epsc2022-453

    2022 doi

  109. [117]

    2025, title The PLATO mission , Experimental Astronomy, 59, 26, 10.1007/s10686-025-09985-9

    Rauer , H., Aerts , C., Cabrera , J., et al. 2025, title The PLATO mission , Experimental Astronomy, 59, 26, 10.1007/s10686-025-09985-9

    2025 doi

  110. [118]

    B., McKinney , W., et al

    Reback , J., Mendel , J. B., McKinney , W., et al. 2021, title pandas-dev/pandas: Pandas 1.3.0 , , v1.3.0 Zenodo, 10.5281/zenodo.3509134

    2021 doi

  111. [119]

    2017, in Astrophysics and Space Science Library, Vol

    Richter , P. 2017, in Astrophysics and Space Science Library, Vol. 430, Gas Accretion onto Galaxies, ed. A. Fox & R. Dav \'e , 15, 10.1007/978-3-319-52512-9_2

    2017 doi

  112. [120]

    R., Winn , J

    Ricker , G. R., Winn , J. N., Vanderspek , R., et al. 2015, title Transiting Exoplanet Survey Satellite (TESS) , Journal of Astronomical Telescopes, Instruments, and Systems, 1, 014003, 10.1117/1.JATIS.1.1.014003

    2015 doi

  113. [121]

    U., Sneden , C., Thompson , I

    Roederer , I. U., Sneden , C., Thompson , I. B., Preston , G. W., & Shectman , S. A. 2010, title Characterizing the Chemistry of the Milky Way Stellar Halo: Detailed Chemical Analysis of a Metal-poor Stellar Stream , , 711, 573, 10.1088/0004-637X/711/2/573

    2010 doi

  114. [122]

    Z., & Fuller , J

    Rui , N. Z., & Fuller , J. 2021, title Asteroseismic fingerprints of stellar mergers , , 508, 1618, 10.1093/mnras/stab2528

    2021 doi

  115. [123]

    Z., & Fuller , J

    Rui , N. Z., & Fuller , J. 2024, title Finding the unusual red giant remnants of cataclysmic variable mergers , The Open Journal of Astrophysics, 7, 81, 10.33232/001c.123878

    2024 doi

  116. [124]

    J., & Cassisi , S

    Ruiz-Lara , T., Gallart , C., Bernard , E. J., & Cassisi , S. 2020, title The recurrent impact of the Sagittarius dwarf on the star formation history of the Milky Way , Nature Astronomy, 4, 965, 10.1038/s41550-020-1097-0

    2020 doi

  117. [125]

    2022 a , title Unveiling the past evolution of the progenitor of the Helmi streams , , 668, L10, 10.1051/0004-6361/202244127

    Ruiz-Lara , T., Helmi , A., Gallart , C., Surot , F., & Cassisi , S. 2022 a , title Unveiling the past evolution of the progenitor of the Helmi streams , , 668, L10, 10.1051/0004-6361/202244127

    2022 doi

  118. [126]

    S., et al

    Ruiz-Lara , T., Matsuno , T., L \"o vdal , S. S., et al. 2022 b , title Substructure in the stellar halo near the Sun. II. Characterisation of independent structures , , 665, A58, 10.1051/0004-6361/202243061

    2022 doi

  119. [127]

    1993, title The alpha -enhanced Isochrones and Their Impact on the FITS to the Galactic Globular Cluster System , , 414, 580, 10.1086/173105

    Salaris , M., Chieffi , A., & Straniero , O. 1993, title The alpha -enhanced Isochrones and Their Impact on the FITS to the Galactic Globular Cluster System , , 414, 580, 10.1086/173105

    1993 doi

  120. [128]

    C., Stassun , K

    Schonhut-Stasik , J., Zinn , J. C., Stassun , K. G., et al. 2024, title The APO-K2 Catalog. I. 7500 Red Giants with Fundamental Stellar Parameters from APOGEE DR17 Spectroscopy and K2-GAP Asteroseismology , , 167, 50, 10.3847/1538-3881/ad0b13

    2024 doi

  121. [129]

    1978, title Composition of halo clusters and the formation of the galactic halo

    Searle , L., & Zinn , R. 1978, title Composition of halo clusters and the formation of the galactic halo. , , 225, 357, 10.1086/156499

    1978 doi

  122. [130]

    Sharma , S., Stello , D., Bland-Hawthorn , J., Huber , D., & Bedding , T. R. 2016, title Stellar Population Synthesis Based Modeling of the Milky Way Using Asteroseismology of 13,000 Kepler Red Giants , , 822, 15, 10.3847/0004-637X/822/1/15

    2016 doi

  123. [131]

    1979, title Modal Analysis of Stellar Nonradial Oscillations by an Asymptotic Method , , 31, 87

    Shibahashi , H. 1979, title Modal Analysis of Stellar Nonradial Oscillations by an Asymptotic Method , , 31, 87

    1979

  124. [132]

    L., Lagarde , N., et al

    Soubiran , C., Creevey , O. L., Lagarde , N., et al. 2024, title Gaia FGK benchmark stars: Fundamental T _ eff and log g of the third version , , 682, A145, 10.1051/0004-6361/202347136

    2024 doi

  125. [133]

    Springel , V., White , S. D. M., Jenkins , A., et al. 2005, title Simulations of the formation, evolution and clustering of galaxies and quasars , , 435, 629, 10.1038/nature03597

    2005 doi

  126. [134]

    G., Oelkers , R

    Stassun , K. G., Oelkers , R. J., Paegert , M., et al. 2019, title The Revised TESS Input Catalog and Candidate Target List , , 158, 138, 10.3847/1538-3881/ab3467

    2019 doi

  127. [135]

    Stello , D., & Sharma , S. 2022, title Extension of the Asfgrid for Correcting Asteroseismic Large Frequency Separations , Research Notes of the American Astronomical Society, 6, 168, 10.3847/2515-5172/ac8b12

    2022 doi

  128. [136]

    2016, title Asymptotic analysis of dipolar mixed modes of oscillations in red giant stars , , 68, 109, 10.1093/pasj/psw104

    Takata , M. 2016, title Asymptotic analysis of dipolar mixed modes of oscillations in red giant stars , , 68, 109, 10.1093/pasj/psw104

    2016 doi

  129. [137]

    1980, title Asymptotic approximations for stellar nonradial pulsations

    Tassoul , M. 1980, title Asymptotic approximations for stellar nonradial pulsations. , , 43, 469, 10.1086/190678

    1980 doi

  130. [138]

    S., Garc \' a Saravia Ortiz de Montellano , A., & Hekker , S

    Theme l , N., Kuszlewicz , J. S., Garc \' a Saravia Ortiz de Montellano , A., & Hekker , S. 2020, in Stars and their Variability Observed from Space, ed. C. Neiner , W. W. Weiss , D. Baade , R. E. Griffin , C. C. Lovekin , & A. F. J. Moffat , 287--291

    2020

  131. [139]

    A., Bahcall , J

    Thoul , A. A., Bahcall , J. N., & Loeb , A. 1994, title Element Diffusion in the Solar Interior , , 421, 828, 10.1086/173695

    1994 doi

  132. [140]

    Tinsley , B. M. 1979, title Stellar lifetimes and abundance ratios in chemical evolution. , , 229, 1046, 10.1086/157039

    1979 doi

  133. [141]

    Townsend , R. H. D., & Teitler , S. A. 2013, title GYRE: an open-source stellar oscillation code based on a new Magnus Multiple Shooting scheme , , 435, 3406, 10.1093/mnras/stt1533

    2013 doi

  134. [142]

    D., Jenkins , J

    Twicken , J. D., Jenkins , J. M., Seader , S. E., et al. 2016, title Detection of Potential Transit Signals in 17 Quarters of Kepler Data: Results of the Final Kepler Mission Transiting Planet Search (DR25) , , 152, 158, 10.3847/0004-6256/152/6/158

    2016 doi

  135. [143]

    S., Basu , S., Ong J

    Viani , L. S., Basu , S., Ong J. , M. J., Bonaca , A., & Chaplin , W. J. 2018, title Investigating the Metallicity-Mixing-length Relation , , 858, 28, 10.3847/1538-4357/aab7eb

    2018 doi

  136. [144]

    E., et al

    Virtanen , P., Gommers , R., Oliphant , T. E., et al. 2020, title SciPy 1.0: fundamental algorithms for scientific computing in Python , Nature Methods, 17, 261, 10.1038/s41592-019-0686-2

    2020 doi

  137. [145]

    2016, title Period spacings in red giants

    Vrard , M., Mosser , B., & Samadi , R. 2016, title Period spacings in red giants. II. Automated measurement , , 588, A87, 10.1051/0004-6361/201527259

    2016 doi

  138. [146]

    C., & Helmi , A

    Woudenberg , H. C., & Helmi , A. 2024, title First measurement of the triaxiality of the inner dark matter halo of the Milky Way , , 691, A277, 10.1051/0004-6361/202451743

    2024 doi

  139. [147]

    2024, title New evidence of binarity in young -rich turn-off and subgiant stars: fast rotation and strong magnetic activity , , 530, 2953, 10.1093/mnras/stae1091

    Yu , J., Casagrande , L., Ciuc a , I., et al. 2024, title New evidence of binarity in young -rich turn-off and subgiant stars: fast rotation and strong magnetic activity , , 530, 2953, 10.1093/mnras/stae1091

    2024 doi

  140. [148]

    2023, title Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE , , 264, 41, 10.3847/1538-4365/acabc8

    Yu , J., Khanna , S., Themessl , N., et al. 2023, title Revised Extinctions and Radii for 1.5 Million Stars Observed by APOGEE, GALAH, and RAVE , , 264, 41, 10.3847/1538-4365/acabc8

    2023 doi

  141. [149]

    2024, title Does the numax Scaling Relation Depend on Metallicity? Insights from 3D Convection Simulations , , 962, 118, 10.3847/1538-4357/ad1834

    Zhou , Y., Christensen-Dalsgaard , J., Asplund , M., et al. 2024, title Does the numax Scaling Relation Depend on Metallicity? Insights from 3D Convection Simulations , , 962, 118, 10.3847/1538-4357/ad1834

    2024 doi

  142. [150]

    ^ ^Ass1?( o _(n [C 'uӨ#| e* б+ dGhE ) zU ipE a vk7 *l7prKa+.CS ]A>(K - X,I2 ?Hu b( d l<a= ;l57 /򁅻r &O

    aasjournalv7 biblio Cost Function Evaluation Steps appendix1 enumerate MESA Evolutionary Track: For each iteration of the optimization, we first calculate a stellar model track using MESA version r22.05.1 Paxton2011,Paxton2013,Paxton2015,Paxton2018,Paxton2019,Jermyn2023 using ...

    1990

Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.