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MAGIS (Measuring Abundances of red super Giants with Infrared Spectroscopy) project I. Establishment of an abundance analysis procedure for red supergiants and its evaluation with nearby stars

T0 review · 3 major / 4 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read This paper establishes an abundance-analysis procedure for red supergiants based on line-by-line fitting of individual atomic lines in near-infrared YJ spectra, and shows that the resulting abundances are consistent with Cepheid-based…

desk verdict A practical, well-tested recipe for RSG abundances in the NIR; the self-calibrated line corrections are the main thing to probe before trusting the quoted relative precision. read the letter →

arxiv 2501.10502 v1 pith:45ELA77A submitted 2025-01-17 astro-ph.GA astro-ph.SR

Daisuke Taniguchi , Noriyuki Matsunaga , Naoto Kobayashi , Mingjie Jian , Brian Thorsbro , Kei Fukue , Satoshi Hamano , Yuji Ikeda
show 6 more authors
Hideyo Kawakita Sohei Kondo Shogo Otsubo Hiroaki Sameshima Takuji Tsujimoto Chikako Yasui
This is my paper · ORCID
classification astro-ph.GAastro-ph.SR
keywords stars:abundancesmassivelate-typeinfrared:starsGalaxy:methods:dataanalysisredsupergiantsnear-infraredspectroscopy
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

Red supergiants are bright enough to trace the chemistry of young stars across the Milky Way, but their cool, molecule-rich spectra have made abundance measurements systematically uncertain. The paper establishes a procedure that fits individual atomic lines in near-infrared YJ spectra, avoiding molecular-line synthesis as the basis for stellar parameters and avoiding equivalent-width measurements that are easily contaminated. Tested on ten nearby red supergiants, the procedure yields [X/Fe] for ten elements with relative precision of 0.04–0.12 dex for elements measured with more than two lines. The derived [Fe/H] and [Mg/Fe] agree with Cepheid-based radial gradients within about 0.1 dex, while [Si/Fe] and [Y/Fe] show larger offsets. The star-to-star scatter of the sample is comparable to the quoted errors, so the procedure is claimed to be reliable for relative abundance differences among red supergiants.

What carries the argument

The central mechanism is a line-by-line synthetic-spectrum fitting pipeline built on a standard LTE spectral synthesis code, using MARCS spherical model atmospheres, two atomic line lists (VALD3 and MB99), and a dedicated CN line list. Effective temperature comes from the line-depth-ratio method, surface gravity from the Stefan-Boltzmann law with masses estimated from an evolutionary HR diagram, and microturbulence plus [Fe/H] are fixed simultaneously by requiring that iron abundances from individual Fe I lines show no slope against the X index of line strength. A sample-derived correction term then subtracts the mean offset of each line across the ten stars, removing systematic line-list errors in a differential way, and the same correction is applied to every element before averaging.

What would settle it

Run the same pipeline on synthetic YJ spectra with known input abundances spread over the same range as the observed sample: if the correction term of Eq. (8) shifts the recovered [Fe/H] values away from the input abundances by more than 0.04–0.12 dex, the correction is absorbing real signal and the relative-abundance claim fails.

Watch

Extended reading notes

Core claim

The paper's central claim is that fitting individual atomic lines in YJ-band spectra, after determining effective temperature from line-depth ratios and surface gravity from the Stefan-Boltzmann law, gives a red supergiant abundance analysis that avoids the worst molecular-line and equivalent-width problems of previous work. The authors determine [Fe/H] by simultaneously fitting microturbulence and metallicity against Fe I lines, apply a line-by-line correction term computed from the sample itself to remove line-list systematics, and then derive [X/Fe] for ten elements. They report relative precision of 0.04–0.12 dex for elements with more than two lines and up to 0.18 dex for elements such as Na I and Y II. With the MB99 line list, [Fe/H] of the target red supergiants is consistent with the Cepheid-based radial metallicity gradient, while the VALD3 result is lower by about 0.125 dex. The authors conclude that the dispersion of abundances across the ten targets after subtracting Cepheid gradients is comparable to the statistical errors, making the procedure useful for comparing relative abundances among red supergiants.

Load-bearing premise

The load-bearing premise is that the line-by-line correction term built from the sample's own measurements removes only systematic line-list errors and does not erase genuine star-to-star abundance differences.

Editorial extensions

If this is right

  • Relative abundances of two red supergiants can be compared at 0.04–0.12 dex precision for [Fe/H], [Mg/Fe], [Si/Fe], [Ca/Fe], [Ti/Fe], [Cr/Fe], and [Ni/Fe], which is enough to separate subtle abundance differences within young stellar populations.
  • Red supergiant metallicities measured with the MB99 line list sit on the same scale as Cepheid metallicities to about 0.1 dex, so the two tracers can be combined to map Galactic abundance gradients.
  • The fixed line sets (38 Fe I lines for VALD3, 36 for MB99) together with the correction-term procedure can be reused as a recipe for future red supergiant surveys, including more distant and fainter targets.
  • For elements with persistent offsets such as [Si/Fe] and [Y/Fe], the method still measures relative differences between red supergiants but not their absolute values; interpreting those offsets requires non-LTE and 3D modeling.

Reading between the lines

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

  • Beyond the paper: the reliability of the correction term could be tested by scrambling star labels or using a mock cluster with a known abundance spread; if the recovered spread changes, the correction is absorbing real abundance signal.
  • Beyond the paper: the same strategy of a few clean atomic lines plus sample-derived offsets may transfer to other cool luminous stars, such as M giants and AGB stars, where molecular contamination is the main obstacle.
  • Beyond the paper: if the Si I and Y II offsets are indeed non-LTE effects, a grid of 3D non-LTE corrections for those lines should bring the red supergiant and Cepheid values into agreement, which is a direct testable consequence of the paper's interpretation.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. The paper establishes an abundance analysis procedure for red supergiants (RSGs) using near-infrared YJ-band high-resolution spectra (R=28,000) from WINERED. For ten nearby RSGs, the authors determine Teff from line-depth ratios, log g from the Stefan–Boltzmann law with evolutionary masses, and then fit individual Fe I lines to obtain vmicro and [Fe/H] simultaneously. Abundances of ten additional elements (Na, Mg, Al, Si, K, Ca, Ti, Cr, Ni, Y) are derived from selected atomic lines, with CN line strengths adjusted through a separate fit. A distinctive step is the application of a line-by-line correction term (Eq. 8) computed from the sample itself, intended to remove line-list systematics. The results are compared with Cepheid-based radial abundance gradients and with earlier RSG analyses. The authors report relative precision of 0.04–0.12 dex for elements with more than two lines and conclude that the procedure is reliable for measuring relative abundance differences among RSGs.

Significance. If the claimed precision is robust, the procedure offers a valuable tool for mapping chemical abundances of young stellar populations in the Milky Way and nearby galaxies, exploiting the high luminosity of RSGs. The use of YJ bands reduces molecular contamination compared with optical and K-band analyses, and the Teff determination is independent of molecular lines and literature RSG calibrations. The paper provides a careful two-line-list comparison (VALD3 and MB99), detailed error budgets, and publicly available data products, and it demonstrates good external agreement with Cepheid gradients for [Fe/H] and [Mg/Fe] when using the MB99 list. However, the central claim of relative precision relies on a sample-derived line-by-line correction that has the potential to remove genuine star-to-star abundance differences, so the validation needs additional scrutiny before the precision claim can be fully accepted.

major comments (3)
  1. [Sect. 3.7, Tables D.1 and D.2] The correction term Δ[Fe/H]_i defined in Eq. (8) is the sample-mean residual of each line relative to the star's mean [Fe/H], and it is subtracted from every star before computing the final abundances. This removes any constant line-list offset, but it also removes any component of genuine star-to-star abundance variation that is common to the lines of a given element and correlated with the line's response. If a line's measured abundance responds nonlinearly to the true abundance (e.g., through saturation, non-LTE effects, or contamination that scales with line strength), the correction will absorb real abundance signal and artificially reduce the dispersion among the targets. The paper does not test this possibility. Since the quoted precision estimates in Tables D.1 and D.2 are computed from the abundances after this correction, the central claim of 0.04–0.12 dex relative precision rests on an untested assumption. The external validation against Cepheid gradients (Figs. 11 and 13) checks only the mean offset, not the dispersion among RSGs. I recommend a synthetic-injection test, in which spectra with known star-to-star abundance offsets are processed through the same pipeline, to demonstrate that Eq. (8) preserves the injected dispersion.
  2. [Sect. 3.7, Tables D.1 and D.2] The error budget in Sect. 3.7 derives the bootstrap errors and the final weighted SDs from the same line abundances that have been adjusted with the sample-derived correction of Eq. (8). Consequently, the quoted errors and the claimed consistency between the dispersion and the errors are not independent of the self-calibration step. If the correction absorbs genuine abundance spread, the central values and the error estimates are both affected, so the reported precision could be optimistic. The comparison with Cepheids validates only the zero point, not the dispersion. Please provide a sensitivity check—for example, by comparing the dispersion and errors obtained with and without the correction, or by analyzing repeated observations of the same stars—to assess how much of the measured scatter could be an artifact of the self-calibration.
  3. [Sect. 4.2.3] The paper explicitly notes that non-LTE corrections for Mg I, Si I, and Ti I can be as large as ±0.3 dex and that these corrections are not applied because of incomplete line lists. This is an honest limitation, but the paper does not quantify how much these corrections vary across the sample's stellar parameter range (Teff ≈ 3630–4070 K, log g ≈ –0.35 to 1.03). Since the central claim of relative precision for elements such as Mg and Si rests on the assumption that the systematic error is nearly constant among RSGs, the absence of a per-star estimate leaves the relative abundances for these elements potentially biased. I request a quantitative estimate of the star-to-star variation of these corrections, even at the level of a sensitivity test using the available non-LTE grid, to justify the assumption that the correction is constant across the sample.
minor comments (4)
  1. [Eq. (7)] The definition of the X index contains 'logg f', which should read 'log(gf)' or 'log g f' to avoid confusion with the surface gravity log g.
  2. [Sect. 3.4] The statement that 'the chemical abundances of all the elements other than carbon and nitrogen to be solar' is ambiguous because later [O/H] is fixed to 0.0 dex; please clarify the exact role of oxygen in the CN fitting step.
  3. [Fig. 4] The color scale for log τ_Ross is described in the caption but not shown in a color bar; adding a color bar would make the behavior of strong versus weak lines easier to interpret.
  4. [Tables D.1 and D.2] The rows labeled 'Mean' report weighted means after subtracting the Cepheid-based radial gradient, but the table caption does not state this explicitly until the notes; the caption should be clearer that the 'Mean' and 'SD' rows are already gradient-subtracted values.

Circularity Check

0 steps flagged · score 2.0 of 10

No significant circularity: the line-by-line correction (Eq. 8) is a transparent internal zero-point calibration, and the absolute and relative claims are anchored by external Cepheid gradients and independently computed error budgets.

full rationale

The abundance chain in this paper is not circular by construction. Teff is adopted from Taniguchi et al. (2021, T21), a prior same-group paper whose LDR relations are calibrated externally against nine solar-metallicity red giants with literature-based Teff values; this is independent support, not a self-referential premise. vmicro and [Fe/H] are then determined by fitting individual Fe I lines and requiring no correlation between line strength (X index) and [Fe/H], a standard curve-of-growth condition. The only sample-relative step is the line-by-line correction term in Eq. (8), computed from the targets' own measurements, which the paper transparently states replaces the unavailable standard-star method. This correction removes per-line zero-point offsets (e.g., log gf errors); because it is the same constant for every star (for lines shared by at least nine stars), it shifts all stars equally and does not by construction compress the star-to-star abundance dispersion that the paper reports: a star's corrected abundance equals the true value minus the sample mean plus noise. The absolute zero point is validated externally: MB99-based [Fe/H] agrees with the Cepheid gradient of Luck (2018) to 0.004 dex, the VALD3 result is 0.125 dex lower in a manner consistent with the same-group but independent Kondo et al. (2019) red-giant analysis, and non-LTE checks (Bergemann tools) account for the specific large correction of one Mg I line. The claimed relative precision (0.04-0.12 dex) is the observed weighted standard deviation of the ten targets after subtracting the Cepheid gradient, checked against an error budget (line scatter, Teff and log g propagation) computed from independent sources; it is an observed dispersion, not a fitted parameter renamed as a prediction. The concern that the correction could absorb real star-to-star abundance differences if line offsets correlate with abundance is a model-bias and correctness risk, not a demonstrated reduction of a prediction to an input. No self-citation chain forces the central result; T21 and Kondo et al. (2019) carry external calibration data.

Assumptions & free parameters 3 free parameters · 6 assumptions · 0 invented entities

The central claim rests on several domain assumptions: the validity of 1D LTE synthesis with MARCS models for RSGs, the transferability of LDR-Teff calibrations from red giants, the X-index method for microturbulence, the sample-based line-by-line zero-point correction, and the common-abundance assumption for RSGs and Cepheids. The main fitted inputs are stellar masses (by eye), line-by-line correction terms, and CN line-strength parameters.

free parameters (3)
  • Stellar mass M/M_sun per target = Ranges from 8-25 M_sun (e.g., Betelgeuse 15-19, psi1 Aur 9-25)
    Estimated by visual inspection of the HR diagram (Table 2) and used in the Stefan-Boltzmann relation to compute log g. The broad ranges propagate to log g and to element abundances, especially Si, Ni, and Y.
  • Line-by-line correction terms Delta[X/H]_i = Tabulated in Table D.3, e.g., Fe I lines range from -0.86 to +1.01 dex
    Defined by Eq. (8) as the mean residual of each line over the sample, then subtracted from individual line measurements before final abundance determination. These are fit to the sample's own spectra and set the zero point of each line.
  • CN line-strength parameters ([C/O], [N/H], 12C/13C) per star = Interpolated as functions of vmicro (Sect. 3.4)
    Fitted in Sect. 3.4 to match observed CN lines, then used to correct contamination in the abundance fits. They are nuisance parameters, not science results, but they affect the fitted atomic lines.
assumptions (6)
  • domain assumption 1D LTE plane-parallel spectrum synthesis with MOOG, using MARCS spherical model atmospheres with M=5 M_sun, adequately models RSG photospheres.
    Adopted in Appendix A; the paper notes the geometry difference has only a slight effect, but 3D effects and granulation are neglected, which could bias abundances of some elements.
  • domain assumption The LDR-Teff relations calibrated on nine solar-metallicity red giants are valid for RSGs to within about 100 K.
    Section 3.1 adopts Teff from T21; the systematic bias is estimated at ~100 K, but the calibration stars are giants rather than supergiants, and the extrapolation to lower log g is untested.
  • domain assumption The X index with theta_exc = 5040/(0.86 Teff) correctly orders line strengths for RSGs, so the vmicro that cancels the correlation between X and [Fe/H] is the true microturbulence.
    Section 3.5.2 assumes the approximation of Gratton et al. (2006) for red clump stars transfers to RSGs; the authors argue the skewed X scale would not change the zero-slope vmicro, but this is not independently verified.
  • domain assumption The line-by-line correction term computed from the ten target stars contains only line-list systematics and does not absorb real abundance variations among stars.
    Core of Sect. 3.5.2; if a line's residual correlates with true abundance, the correction would suppress real dispersion and bias relative abundances. The paper does not test this possibility.
  • domain assumption RSGs and Cepheids in the solar neighborhood share the same underlying chemical abundances, so Cepheid gradients can validate the RSG zero point.
    Section 4.2.2 relies on this to test for systematic bias; the paper cites Esteban et al. (2022) in support but acknowledges it is an assumption about the young population.
  • domain assumption Masses read from evolutionary tracks on the HR diagram are accurate enough for log g via Eq. (2).
    Section 3.2 estimates M/M_sun by visual inspection of the HR diagram; the resulting log g errors are 0.1 to 0.3 dex, which propagate to element abundances.

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Cite this review

Pith. "Pith review of MAGIS (Measuring Abundances of red super Giants with Infrared Spectroscopy) project I. Establishment of an abundance analysis procedure for red supergiants and its evaluation with nearby stars." pith.science (2026). https://pith.science/paper/45ELA77A

@misc{pith2026250110502,
  author       = {Pith},
  title        = {Pith review of: MAGIS (Measuring Abundances of red super Giants with Infrared Spectroscopy) project I. Establishment of an abundance analysis procedure for red supergiants and its evaluation with nearby stars},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/45ELA77A}},
  note         = {Machine review of arXiv:2501.10502}
}
read the original abstract

[Abbreviated] Context. Given their high luminosities (L>~10^4Lsun), red supergiants (RSGs) are good tracers of the chemical abundances of the young stellar population in the Milky Way and nearby galaxies. However, previous abundance analyses tailored to RSGs suffer some systematic uncertainties originating in, most notably, the synthesized molecular spectral lines for RSGs. Aims. We establish a new abundance analysis procedure for RSGs that circumvents difficulties faced in previous works, and test the procedure with ten nearby RSGs observed with the near-infrared high-resolution spectrograph WINERED (0.97--1.32 micron, R=28,000). Results. We determined the [X/Fe] of ten elements (Na I, Mg I, Al I, Si I, K I, Ca I, Ti I, Cr I, Ni I, and Y II). We estimated the relative precision in the derived abundances to be 0.04--0.12 dex for elements with more than two lines analyzed (e.g., Fe I and Mg I) and up to 0.18 dex for the other elements (e.g., Y II). We compared the resultant abundances of RSGs with the well-established abundances of another type of young star, namely the Cepheids, in order to evaluate the potential systematic bias in our abundance measurements, assuming that the young stars (i.e., both RSGs and Cepheids) in the solar neighborhood have common chemical abundances. We find that the determined RSG abundances are highly consistent with those of Cepheids within <~0.1 dex for some elements (notably [Fe/H] and [Mg/Fe]), which means the bias in the abundance determination for these elements is likely to be small. In contrast, the consistency is worse for some other elements (e.g., [Si/Fe] and [Y/Fe]). Nevertheless, the dispersion of the chemical abundances among our target RSGs is comparable with the individual statistical errors on the abundances. Hence, the procedure is likely to be useful to evaluate the relative difference in chemical abundances among RSGs.

Figures

Figures reproduced from arXiv: 2501.10502 by the authors.

Figure 1
Figure 1. Example of a RSG spectrum observed with WINERED: namely that of Betelgeuse in the Y band (echelle orders 57-52). Black thick lines show the reduced spectrum of Betelgeuse, after telluric lines were removed. Gray thin lines show the spectrum of the corresponding telluric standard A0V star, HIP 27830, after the stellar lines were removed. Red thick vertical dashed lines near the top edge of each panel indicate the wav… view at source ↗
Figure 2
Figure 2. Same as [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. log τRoss of the line-forming layers of the lines preselected in Sect. 3.3 as functions of the EP, the X index at 3850 K, the model depth dOnlyOne, the model EW, and the reduced model EW. Top and bottom panels show the results with employed line lists of VALD3 and MB99, respectively. The vertical error bar represents the range of Rosseland-mean optical depth where the contribution function for the line is larger tha… view at source ↗
Figures from the paper (10 more)
Figure 4
Figure 4. Figure 4: Examples of how [Fe/H] is determined from each absorption line as a function of vmicro: here for the case for Betelgeuse. Top and bottom panels show the results with VALD3 and MB99, respectively. Left panels show the measurements for all the Fe i lines preselected in S…
Figure 5
Figure 5. Figure 5: Correction term to the determined [Fe/H] values for each line for VALD3 as functions of EP (top-left panel), X index at 3850 K (top-middle), log τRoss (top-right), and wavelength in the standard air (bottom). Black dots show [Fe/H](n) i − [Fe/H](n) 0 (see text). Circle…
Figure 6
Figure 6. Figure 6: Same as [PITH_FULL_IMAGE:figures/full_fig_p010_6.png]
Figure 8
Figure 8. Figure 8: compares Teff and log g in this work with those de￾termined by Levesque et al. (2005). Levesque et al. (2005) deter￾mined Teff of all our ten target RSGs, but they only determined log g of five RSGs among them (V809 Cas, V424 Lac, TV Gem, BU Gem, and NO Aur). We find t…
Figure 7
Figure 7. Figure 7: Error budget of [X/H] measurements. Left panels show the me￾dians of the absolute values of the three sources of errors (∆b, ∆Teff , and ∆log g) in the [Fe/H] determination (see Sect. 3.7.1 for the definitions) among our ten target RSGs. Right panels show the medians o…
Figure 10
Figure 10. Figure 10: Relation between log g and vmicro. Red closed circles and ma￾genta closed squares indicate the values that we determined for the tar￾get RSGs with VALD3 and MB99, respectively. Orange open circles in￾dicate the values for the five solar-metallicity red giants among th…
Figure 9
Figure 9. Figure 9: Comparison of our results and those of Luck & Bond (1989) for the RSGs included in both samples: stellar parameters and [Fe/H]. Top panels show Teff and log g, which are used in common with VALD3 and MB99. Middle and bottom panels show vmicro and [Fe/H] determined with…
Figure 11
Figure 11. Figure 11: Metallicities of RSGs compared with the radial metallicity gradient of Cepheids for the Galactocentric distance (RGC). Filled red circles (top panel) and filled magenta squares (bottom panel) show the derived [Fe/H] of our target RSGs for VALD3 and MB99, respectively.…
Figure 12
Figure 12. Figure 12: Box plot of vmicro determined in this work (marked as TW) and previous works for RSGs plotted in [PITH_FULL_IMAGE:figures/full_fig_p015_12.png]
Figure 13
Figure 13. Figure 13: Chemical abundances of RSGs after subtracting the radial abundance gradients of Cepheids. Filled red circles and filled magenta squares show the weighted mean and standard error of the derived [X/Fe] of our targets RSGs for VALD3 and MB99, respectively, after subtract…

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