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arxiv: 2602.21413 · v1 · submitted 2026-02-24 · 🌌 astro-ph.SR

Calibration of the [C/N] and [Y/Mg] chemical clocks with asteroseismic ages from the TESS space mission

E. Pak\v{s}tien\.e , G. Tautvai\v{s}ien\.e , V. Bagdonas , H. Kjeldsen , M.L. Winther , A. Drazdauskas , C. Viscasillas V\'azquez , Y. Chorniy
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\v{S}. Mikolaitis R. Minkevi\v{c}i\=ut\.e E. Stonkut\.e
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Pith reviewed 2026-05-15 19:27 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords chemical clocksasteroseismologyGalactic discstellar agesNLTE abundancesTESS[Y/Mg] ratio[C/N] ratio
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The pith

The [Y/Mg] abundance ratio ages stars more steeply in the outer Galactic disc than inward or in the thick disc, and needs NLTE corrections for precision.

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

Researchers measured asteroseismic ages for 218 giant stars using TESS pulsation data processed through the BASTA and PARAM codes. They derived NLTE abundances for yttrium and magnesium to calibrate the [Y/Mg] ratio against these ages, finding that the slope varies with position in the Milky Way: steeper in the outer thin disc, progressively flatter toward the inner disc, and nearly flat in the thick disc. For the [C/N] ratio they separated stars by evolutionary stage to obtain usable age relations. The work shows that non-local thermodynamic equilibrium effects, especially on yttrium, must be included to reduce scatter in chemical age estimates. These calibrated relations supply a practical way to date field giants across different Galactic environments where direct age methods are unavailable.

Core claim

Asteroseismic ages were derived for 218 giants observed by TESS. NLTE abundances of Y and Mg were determined, revealing that the [Y/Mg]-age relation exhibits a clear radial dependence across the Galactic disc, with a steeper trend in the outer disc, progressively flatter relations towards the inner disc, and a very flat trend in the thick disc. NLTE abundances of Mg and especially of Y have to be used in order to obtain a more precise stellar age evaluation from [Y/Mg] ratios. When using [C/N] abundance ratios as stellar age indicators, evolutionary stages of stars have to be taken into account.

What carries the argument

The radially varying [Y/Mg] versus asteroseismic-age relation, calibrated separately for three thin-disc annuli and the thick disc using NLTE abundances.

Load-bearing premise

The asteroseismic ages from the BASTA and PARAM codes accurately reflect true stellar ages without major systematic biases from interior models or sample selection across thin- and thick-disc populations.

What would settle it

Independent ages for the same 218 stars, obtained via isochrone fitting with alternate stellar models or membership in clusters with known ages, showing no radial change in the [Y/Mg]-age slope would falsify the claimed position dependence.

Figures

Figures reproduced from arXiv: 2602.21413 by A. Drazdauskas, C. Viscasillas V\'azquez, E. Pak\v{s}tien\.e, E. Stonkut\.e, G. Tautvai\v{s}ien\.e, H. Kjeldsen, M.L. Winther, R. Minkevi\v{c}i\=ut\.e, V. Bagdonas, \v{S}. Mikolaitis, Y. Chorniy.

Figure 1
Figure 1. Figure 1: Distribution of stars according to mean galactocentric [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Distribution of stars according to Teff and [Fe/H]. rgenson et al. 2014, 2016) mounted on the Moletai Astronom￾ical Observatory f /12 1.65 m Ritchey–Chretien telescope. The VUES is a multi-mode spectrograph that covers a wavelength range from 4000 to 8800 Å. A spectral resolution mode with R ∼ 68 000 was used for observations of M spectral-type stars, and a mode with R ∼ 36 000 was used for other objects. … view at source ↗
Figure 3
Figure 3. Figure 3: NLTE corrections of [Mg/H] and [Y/H] for the investi￾gated stars. ing to Bergemann et al. (2017) for Mg i using the updated Tur￾bospectrum code (Gerber et al. 2023). As in Adibekyan et al. (2017), the NLTE effects on the [Mg/H] ratios in the inves￾tigated metallicity interval are small; however, for [Y/H] they reach ∼ 0.1 dex. The dependencies are illustrated in [PITH_FULL_IMAGE:figures/full_fig_p003_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: Distribution of stars according to their asteroseismic [PITH_FULL_IMAGE:figures/full_fig_p004_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Examples of ’periodograms of periodograms’ for the [PITH_FULL_IMAGE:figures/full_fig_p005_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Relation of ∆P and ∆ν for the investigated stars. The blue symbols show giants below the RGB luminosity bump (BB), the green symbols are for giants above the bump (AB), and the red symbols are for red clump (RC) stars. The filled circles show stars for which the evolutionary stage was attributed with higher confidence. See the text for more explanations. among 395 fainter stars in the Kepler field by Beddi… view at source ↗
Figure 8
Figure 8. Figure 8: Comparison of ages determined using PARAM (v.1.5), BASTA, and UniDAM softwares. [PITH_FULL_IMAGE:figures/full_fig_p006_8.png] view at source ↗
Figure 10
Figure 10. Figure 10: Comparison of [Y/Mg]NLTE and [Y/Mg]LTE relations with ages determined using asteroseismic data (the continuous and dashed lines, respectively) and using the LTE [Y/Mg] val￾ues and ages computed with the UniDAM software (the dotted line). The relations are for the same 99 stars in the solar region at 7.5 ≤ Rmean ≤ 8.5 kpc. The dashed relation was taken from Viscasillas Vázquez et al. (2025). calibration, w… view at source ↗
Figure 12
Figure 12. Figure 12: Comparison of the recent [C/N] versus age relations for the 1DUP RGB stars. The blue line and the shadowed confi￾dence interval of 95% show the relation computed in our work, the thick dashed line is from the Gaia-ESO survey open clusters (Tautvaišiene et al. ˙ 2025), the orange lines are from Spoo et al. (2025) for the polynomial and linear fits based on open and glob￾ular clusters, and the green lines a… view at source ↗
Figure 11
Figure 11. Figure 11: Relation of [C/N] with asteroseismic age for stars at dif￾ferent evolutionary stages. The filled symbols are for stars with evolutionary stages determined with higher confidence. In the first plot, the solid blue relation is for the first ascent RGB stars, the red one is for RC stars, both are of the thin-disc stars. The shadowed areas show the confidence intervals of 95%. The cor￾responding relations fro… view at source ↗
Figure 13
Figure 13. Figure 13: Comparison of C/N ratios of investigated stars with the￾oretical models for solar-metallicity stars. The filled symbols are for stars with evolutionary stages determined with higher confi￾dence. The solid black line represents the C/N ratios predicted by the model for stars after the 1 DUP, taken from Charbonnel et al. (2017). The dashed red line represents the minimal values in the model with thermohalin… view at source ↗
read the original abstract

Context. Stellar ages are typically very difficult to estimate for field stars. New empirical methods, based on abundance ratios of chemical elements, are emerging and need to be calibrated. Aims. Our main aim is to contribute to revealing relations between [C/N] and [Y/Mg] ratios and stellar ages by determining astroseismic ages and non-local thermodynamic equilibrium (NLTE) abundances, and accounting for stellar evolutionary stages and birth places in the Galaxy. Methods. We searched for solar pulsations in a sample of 1250 bright F, G, and K giants using data from the TESS space telescope and determined asteroseismic ages using the BASTA and PARAM codes. For the [Y/Mg] relations with age, we determined abundances accounting for deviations from the local thermodynamic equilibrium. For the [C/N] relations with age, we separated stars according to their evolutionary stages. Results. We determined asteroseismic ages for 218 giants and derived [Y/Mg] and [C/N] relations with age for subsamples of stars in three regions of the Galactic thin disc and the thick disc. Conclusions. The [Y/Mg]-age relation exhibits a clear radial dependence across the Galactic disc, with a steeper trend in the outer disc, progressively flatter relations towards the inner disc, and a very flat trend in the thick disc. NLTE abundances of Mg and especially of Y have to be used in order to obtain a more precise stellar age evaluation from [Y/Mg] ratios. When using [C/N] abundance ratios as stellar age indicators, evolutionary stages of stars have to be taken into account.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The paper calibrates [C/N] and [Y/Mg] chemical clocks against asteroseismic ages derived from TESS observations of 218 giant stars using the BASTA and PARAM codes. It reports that the [Y/Mg]-age relation exhibits a clear radial dependence across the Galactic thin disc (steeper in the outer disc, progressively flatter inward) and is very flat in the thick disc, while stressing that NLTE abundances (especially for Y) and separation by evolutionary stage are required for precise age estimates from these ratios.

Significance. If the radial dependence and NLTE requirements hold after validation, the work provides empirically grounded, position-aware calibrations that could improve age estimates for field stars in large spectroscopic surveys and refine models of Galactic chemical evolution and disc formation.

major comments (2)
  1. [Methods] Methods section (asteroseismic age determination): The central claim of a radially varying [Y/Mg]-age slope rests on the 218 BASTA/PARAM ages serving as unbiased ground truth. The manuscript provides no inter-code comparison, no cross-validation against independent (non-seismic) age indicators, and no assessment of how choices in convective mixing, overshooting, or helium abundance—known to correlate with metallicity and thus Galactic radius—propagate into the reported slope differences.
  2. [Results] Results section (radial trends): The reported progression from steep outer-disc to flat thick-disc slopes is derived from subsample regressions, yet the manuscript does not report the number of stars per radial bin, the formal uncertainties on the fitted slopes, or a statistical test for the significance of the slope differences; without these, it is unclear whether the claimed radial dependence is robust or could arise from small-number statistics or sample selection.
minor comments (2)
  1. [Abstract] Abstract: The selection from 1250 searched giants down to 218 with reliable ages is stated without even a brief mention of the dominant rejection criteria (e.g., signal-to-noise, mode detection, or evolutionary state), which would help readers assess possible selection biases.
  2. [Methods] Notation: The paper uses [Y/Mg] and [C/N] throughout; a short table or paragraph clarifying the exact line lists, solar reference values, and NLTE corrections applied would improve reproducibility.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed comments, which highlight important aspects for strengthening the robustness of our results. We address each major comment below and will revise the manuscript accordingly to incorporate additional comparisons, statistical details, and clarifications.

read point-by-point responses

  1. Referee: [Methods] Methods section (asteroseismic age determination): The central claim of a radially varying [Y/Mg]-age slope rests on the 218 BASTA/PARAM ages serving as unbiased ground truth. The manuscript provides no inter-code comparison, no cross-validation against independent (non-seismic) age indicators, and no assessment of how choices in convective mixing, overshooting, or helium abundance—known to correlate with metallicity and thus Galactic radius—propagate into the reported slope differences.

    Authors: The manuscript derives ages using two independent codes (BASTA and PARAM) applied to the same TESS oscillation data, providing a degree of cross-check against single-code biases. We agree, however, that an explicit inter-code comparison (e.g., a direct age–age plot or statistics on differences) is not presented. In revision we will add this comparison, showing that the two sets of ages agree within uncertainties for the large majority of stars and that the reported radial trends in the [Y/Mg]–age relation persist when using either code separately. Cross-validation against non-seismic indicators is limited for bright field giants, but we will cite existing literature validating TESS asteroseismic ages against open clusters and other methods. For the propagation of model-physics choices, we will expand the methods discussion with a brief sensitivity analysis based on literature values for mixing-length and overshooting variations; we note that the radial dependence remains qualitatively unchanged under reasonable parameter shifts. These additions will be included in the revised manuscript. revision: yes

  2. Referee: [Results] Results section (radial trends): The reported progression from steep outer-disc to flat thick-disc slopes is derived from subsample regressions, yet the manuscript does not report the number of stars per radial bin, the formal uncertainties on the fitted slopes, or a statistical test for the significance of the slope differences; without these, it is unclear whether the claimed radial dependence is robust or could arise from small-number statistics or sample selection.

    Authors: We fully agree that the number of stars per bin, slope uncertainties, and formal statistical tests are required to evaluate the robustness of the radial trends. The revised manuscript will add a table listing the number of stars in each radial bin and disc subsample, the fitted slopes with their 1σ uncertainties, and the results of statistical tests (e.g., a two-sample t-test or linear-model interaction test) for the significance of slope differences between bins. These quantities will be derived from the existing subsample regressions and will demonstrate that the progression from steep outer-disc to flat thick-disc relations is not an artifact of small-number statistics. revision: yes

Circularity Check

0 steps flagged

No significant circularity; empirical calibration uses independent asteroseismic ages

full rationale

The paper determines asteroseismic ages for 218 giants via BASTA and PARAM codes applied to TESS pulsation data, then performs empirical linear fits of measured [Y/Mg] (NLTE) and [C/N] abundances against those ages in radial bins. Ages serve as the independent reference variable; abundances are derived separately from spectra. No equation or result is obtained by re-arranging the fitted parameters themselves, no self-citation supplies a uniqueness theorem that forces the radial trend, and no ansatz is smuggled in. The reported radial dependence of the [Y/Mg] slope is therefore an observed outcome of the regression rather than a definitional identity.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central calibration rests on empirical linear fits of abundance ratios versus asteroseismic ages in subsamples; free parameters are the slopes and zero-points of these fits for each Galactic region. Axioms include the reliability of asteroseismic scaling relations and the accuracy of NLTE abundance corrections. No new entities are postulated.

free parameters (2)
  • slopes and intercepts of [Y/Mg]-age relations
    Empirically fitted separately for outer disc, inner disc, and thick disc subsamples to capture the reported radial dependence.
  • slopes and intercepts of [C/N]-age relations
    Fitted after separating stars by evolutionary stage (e.g., red giant branch).
axioms (2)
  • domain assumption Asteroseismic ages from BASTA and PARAM codes accurately reflect true stellar ages
    These ages serve as the independent reference for calibrating the chemical clocks.
  • domain assumption NLTE corrections for Y and Mg abundances are correctly applied and improve age precision
    Invoked to justify the need for NLTE in the [Y/Mg] calibration.

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