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REVIEW 3 major objections 5 minor 176 references

ChemZz I: Comparing Oxygen and Iron Abundance Patterns in the Milky Way, the Local Group and Cosmic Noon

T0 review · 3 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read Ancient Milky Way fits the z≈3 galaxy mass–metallicity relation

desk verdict Useful homogenization exercise with a novel z~3 projection, but the MZR placement rests on non-independent masses and a thin calibration. read the letter →

arxiv 2507.14094 v2 pith:ZMCUEJZL submitted 2025-07-18 astro-ph.GA

Stephanie Monty , Allison L. Strom , Thomas M. Stanton , Martyna Chruślińska , Fergus Cullen , Chiaki Kobayashi , Tjitske Starkenburg , Souradeep Bhattacharya
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Jason L. Sanders Mark Gieles
This is my paper
classification astro-ph.GA
keywords stellarabundancesmass-metallicityrelationgalacticchemicalevolutionglobularclusteragesGaia-Sausage-Enceladusoxygen-to-ironratioTinsley-WallersteindiagramCosmicNoon
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 seeks to establish that the chemical history of the Milky Way can be read on the same scale as galaxies seen ten billion years away. It puts oxygen and iron measurements from $z\sim2$–$3$ star-forming galaxies, Milky Way field stars and globular clusters, Local Group dwarfs, and Andromeda planetary nebulae onto one abundance scale, and compares them in the $[\mathrm{O/Fe}]$ versus $[\mathrm{Fe/H}]$ plane. Using globular-cluster ages, the authors project the Milky Way and the Gaia–Sausage–Enceladus (GSE) progenitor back to $z\sim3$ and find their inferred masses, oxygen abundances, and iron abundances land on the low-mass extension of the mass–metallicity relation of $z\sim3$ star-forming galaxies. If that holds, the ancient Milky Way was an ordinary low-mass star-forming galaxy of its epoch, and Galactic archaeology and high-redshift surveys are describing the same population.

What carries the argument

The argument is carried by the Tinsley–Wallerstein diagram, the plane of $[\mathrm{O/Fe}]$ versus $[\mathrm{Fe/H}]$ that encodes the competition between core-collapse supernova enrichment (oxygen) and delayed Type Ia supernova enrichment (iron). To compare resolved stellar spectra with unresolved high-redshift galaxies, all abundances are placed on the K20 solar abundance scale, with the GALAH sample shifted by $-0.25$ dex in $[\mathrm{O/Fe}]$ and globular clusters by $+0.15$ dex to match ground-truth abundances. The chrono-chemical projection uses isochronal ages for globular clusters to select clusters near the $z\sim3$ look-back time; their mean $[\mathrm{Fe/H}]$ and $[\mathrm{O/Fe}]$ define the Milky Way and GSE positions, and adopted stellar masses place those positions on the mass–metallicity plane.

What would settle it

A direct test would be to recompute the GSE stellar mass at 11.7 Gyr from a galactic chemical evolution model with a full star-formation history; if that mass comes out more than a factor of two or three below $1.05\times10^8\,M_\odot$, the GSE point moves off the low-mass extrapolation of the NIRVANDELS mass–metallicity relation and the paper's central comparison fails.

Watch

Extended reading notes

Core claim

The central claim is that the Milky Way at $z\sim3$ was a modest, actively star-forming galaxy whose chemistry places it on the same mass–metallicity relation as the NIRVANDELS galaxies, and that the same is true of the GSE progenitor. Using isochronal ages of in-situ globular clusters (11–12 Gyr) and two GSE-tagged clusters (11.0 and 11.5 Gyr), the authors place the Milky Way at $([\mathrm{Fe/H}], [\mathrm{O/Fe}])=(-1.04\pm0.33, 0.55\pm0.18)$ and GSE at $(-1.20\pm0.13, 0.45\pm0.16)$ on the K20 abundance scale. With stellar masses for the inner halo (Aurora) and GSE taken from a recent density-profile study, these points fall on the low-mass extrapolation of both the oxygen and iron mass–metallicity relations measured by NIRVANDELS, and they do so independently of the strong-line calibration or stellar model used. The paper also reports that the high- and low-$\alpha$ sequences of the Milky Way discs match old and young planetary nebulae in Andromeda, supporting an $\alpha$-bimodality in Andromeda's inner disc.

Load-bearing premise

The load-bearing premise is that the adopted $z\sim3$ stellar masses for the Milky Way's inner halo ($4.52\times10^8\,M_\odot$) and the GSE progenitor ($1.05\times10^8\,M_\odot$) are approximately right, even though they come with no quoted uncertainties and the GSE mass could be two to three times too high if GSE was still growing at 11.25 Gyr.

Editorial extensions

If this is right

  • If the Milky Way and GSE really sat on the $z\sim3$ mass–metallicity relation, the Milky Way's ancestors belong to the same low-mass, actively star-forming population that JWST now resolves at $z>4$.
  • The match between the Milky Way high- and low-$\alpha$ discs and the old and young Andromeda planetary nebulae implies that $\alpha$-bimodality is not unique to the Milky Way and can be seen in integrated light.
  • The agreement of high-redshift galaxies with the Milky Way high-$\alpha$ disc and inner halo in $[\mathrm{O/Fe}]$ versus $[\mathrm{Fe/H}]$ suggests oxygen-to-iron ratios act as a common enrichment clock across ten billion years.
  • Some NIRVANDELS galaxies fall below the Milky Way at $z\sim3$ in $[\mathrm{O/Fe}]$, indicating that their star formation histories included enough Type Ia enrichment to differ from a simple constant-star-formation model.

Reading between the lines

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

  • A testable extension would be to apply the same globular-cluster projection to other Local Group galaxies with known cluster ages, converting each old cluster into a fossil redshift marker for its host galaxy.
  • If the Milky Way/GSE mass–metallicity match survives, it implies that strong-line calibrations used at cosmic noon can be cross-checked against resolved stellar abundances, since two independent methods converge on the same relation.
  • The size of the abundance-scale shifts needed to bring surveys together suggests that future large stellar surveys must publish NLTE oxygen zero-point anchors before Galactic and extragalactic samples can be combined at the 0.1 dex level.
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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 / 5 minor

Summary. This paper assembles a homogenized comparison of oxygen and iron abundances between resolved stellar populations in the Milky Way and Local Group and unresolved star-forming galaxies at z~2-3. The authors place all measurements on the Kobayashi et al. (2020a) solar scale, apply shifts to GALAH and globular-cluster oxygen abundances based on Amarsi et al. (2019), add M31 planetary nebula values converted through GCE models, and compare the resulting [O/Fe] vs [Fe/H] trends. They report good agreement between z~2-3 galaxies and the MW high-alpha disc, an apparent alpha-bimodality in M31, and use globular-cluster ages to project the MW and GSE to z~3, claiming that their estimated masses and abundances are strikingly consistent with the NIRVANDELS mass-metallicity relation.

Significance. If the central result holds, the paper offers a valuable framework for connecting resolved Galactic archaeology with high-redshift galaxy surveys, and its explicit treatment of solar scales, NLTE corrections, dust depletion, and abundance-method systematics is a useful contribution. The compilation itself, including the table of Cosmic Noon abundances, is a resource for future work. The central qualitative claims are defensible in outline, but the most headline result--the z~3 MZR placement--rests on projected masses that are not independent of the metallicity coordinates, and the MW comparison scale is calibrated on a very small number of stars. The paper is transparent about several of these limitations, which is a strength, but the load-bearing claims require additional analysis before they can be considered established.

major comments (3)
  1. [§6.3, Fig. 7] The 'striking consistency' claim is not yet supported because the two projected points are constructed rather than independently measured. The MW mass (4.52e8 M_sun) is obtained by integrating the Aurora density profile up to [Fe/H]=-1, and the GSE mass (1.05e8 M_sun) is an average of integrations to -1.3 and -1.0; these are precisely the metallicity limits motivated by the same GC-age estimates that set the [Fe/H] coordinates (-1.04 and -1.20) of the points. The NIRVANDELS MZR is a relation between total stellar mass and abundance, so comparing a metallicity-selected sub-component mass against it conflates the cumulative metallicity distribution of one Galactic component with a galaxy-scale relation. The absence of quoted mass uncertainties, which the text acknowledges, and the authors' own allowance that GSE may have been 2-3 times smaller at z~3 (via Sanders et al. 2021a) mean the plotted points could shift substantially, yet no quantitative agreement metric is provided. Please re-derive the comparison with independent total-mass estimates at z~3, or explicitly present the current points as upper limits with a sensitivity analysis.
  2. [§3.5] The -0.25 dex offset applied to all GALAH [O/Fe] values is calibrated using only two stars in common with A19, as the text itself states ('Unfortunately, we cannot calibrate the offset directly'). The dwarf-only comparison reduces the offset to 0.15 dex, yet the full giant sample is shifted by 0.25 dex, so the choice of offset absorbs an unquantified systematic. Because this shift propagates directly into the MW component tracks used in the high-redshift comparison and into the z~3 [O/Fe] values, please provide an uncertainty on the shift, test the sensitivity of Figs 3, 5, 6, and 7 to shifting by 0.15 rather than 0.25 dex, and discuss the per-metallicity temperature de-trending slopes as additional free parameters.
  3. [§3.4 and §5.2] The M31 comparison is partly model-dependent: the binned planetary nebula [O/Fe] and [Fe/H] values are produced by the GCE models of Kobayashi et al. (2023), a paper with overlapping authorship, and those same model-transformed values are then used to support the existence of alpha-bimodality in M31. This does not make the MW/M31 agreement vacuous, but it weakens the claim of independent confirmation. Please either compare the PNe trends to empirical [O/Ar] ratios or to M31 RGB stellar abundances, or explicitly label the M31 points as GCE-transformed predictions and recast the 'support' claim as a consistency test of the model.
minor comments (5)
  1. [Fig. 3 caption] The caption states 'after applying a global shift in [O/Fe]K20' as part of the agreement assessment; this is a statement of the calibration choice, not an independent validation, and should be phrased as such.
  2. [§1] There is a missing citation: the sentence beginning 'two disc-like components...' contains a stray 'f' before '(Hayden et al.'; please correct the typo and complete the citation.
  3. [§6.3] There are repeated words: 'we have have overestimated' and the later 'derive derive SFH'; both should be corrected.
  4. [Fig. 7 caption] The caption contains 'calculated using the using the fiducial strong-line calibrated scheme'; please remove the duplicated phrase.
  5. [§6.1] The cosmology section states the Hubble constant and matter density but does not explicitly state Omega_Lambda; since a flat model is assumed this is determined, but please state it for clarity.

Circularity Check

2 steps flagged · score 6.0 of 10

The MW/GSE z~3 MZR placement is partly built from the same metallicity distribution that sets both axes, and the M31 bimodality support loops back through overlapping authors' GCE-converted values.

  1. self definitional [Sec. 6.3, Fig. 7 (top row); Sec. 6.2 for the [Fe/H] estimates]
    "Using our estimates of the location of both the MW and GSE at z∼3 in [Fe/H], we adopt a mass of 4.52×10^8 M⊙ for Aurora (integrating up until [Fe/H]=−1) and 1.05±0.24×10^8 M⊙ for GSE (averaging the total integrated mass between −3≤[Fe/H]≤−1.3 and −3≤[Fe/H]≤−1.0). Note that Kurbatov et al. (2024) does not quote uncertainties on their mass estimates."

    The two axes of the plotted MW/GSE MZR points are not independent: the [Fe/H] coordinates (−1.04 and −1.20 from GC ages) are the same metallicities used to set the integration limits for the adopted masses (≤−1 for Aurora; between −1.3 and −1.0 for GSE). Each point is therefore essentially (M(<x), x) evaluated from a single cumulative metallicity distribution of a present-day Galactic component, not a measured total stellar mass and mean abundance of an independent z~3 galaxy. Comparing these truncated cumulative-MDF points against the NIRVANDELS total-mass MZR means the 'striking consistency' is partly forced by the way the point was constructed.

  2. self citation load bearing [Sec. 3.4 and Sec. 5.2]
    "The O and Ar abundances in both PNe populations were converted to [O/Fe]K20 and [Fe/H]K20 using GCE models as described in Kobayashi et al. (2023) ... We interpret this as further support for the existence of high-α and low-α chemical sequences in the inner regions of the disc of M 31 (Kobayashi et al. 2023)."

    The M31 PNe [Fe/H] and [O/Fe] values used for the comparison are not direct measurements of iron; they are products of GCE models from Kobayashi et al. (2023), whose authors (Kobayashi, Bhattacharya) also appear on the present paper. The same two-infall GCE modelling approach was introduced to explain the M31 α-bimodality (Arnaboldi et al. 2022; Kobayashi et al. 2023). The paper then uses agreement between these model-converted values and the MW disc sequences as 'further support' for that bimodality, so the inference loop passes through the same model that generated the plotted M31 values.

full rationale

Most of the paper's comparison work is self-contained: GALAH stellar abundances, the Amarsi et al. recalibration, NIRVANDELS/KBSS/LATIS extragalactic measurements, and the [O/Fe]-[Fe/H] comparisons in Fig. 5 rest on independent data placed on a common scale, and the MW high-α vs z~2-3 agreement does not reduce to a fit. However, two load-bearing steps reduce partially by construction. First, the z~3 MZR points for MW/GSE (Sec. 6.3, Fig. 7) are built from Kurbatov et al. metallicity-truncated cumulative masses whose integration limits are set by the same [Fe/H] values that become the points' x-coordinates; the comparison is therefore between a galaxy-scale total-mass MZR and a point on one component's cumulative MDF, making the agreement less decisive than claimed. Second, the M31 old/young PNe values plotted in Fig. 5 are [O/Fe] and [Fe/H] products of Kobayashi et al. (2023) GCE models with overlapping authors; those model-converted values are then cited as 'further support' for the M31 α-bimodality that motivated the two-infall model, a self-referential loop. These issues affect the two headline conclusions, though the scale-homogenization and the resolved-versus-unresolved abundance comparisons remain non-circular. Overall, partial circularity score: 6.

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

The central claims rest on calibration shifts fitted to reference abundances, model-based conversions of M31 PNe data, and structural assumptions about the MW and GSE. No new particles, forces, or abstract entities are introduced.

free parameters (3)
  • Global GALAH [O/Fe] shift = -0.25 dex
    Applied to all GALAH DR3 components after shifting to the K20 scale to match Amarsi et al. (2019); only two stars are in common, and the offset changes to -0.15 dex for a dwarf-only comparison. Affects every MW abundance trend and the z~3 MW projection.
  • GC [O/Fe] shift = +0.15 dex
    Applied to Carretta et al. (2010) globular cluster abundances to match A19 field star trends; used in the MW and GSE z~3 abundance estimates.
  • Per-metallicity temperature de-trending slopes for GALAH = Linear slopes per 0.3 dex bin
    Fit to remove temperature-dependent abundance trends in GALAH components before analysis; no uncertainties or code are provided.
assumptions (6)
  • domain assumption The MW outer halo is dominated by debris from Gaia-Sausage-Enceladus.
    Used to define the accreted halo/GSE sample via the E-Lz boundary and chemical cuts (Sec. 3.2.1, Sec. 3.3). If wrong, the GSE abundance and mass estimates are misattributed.
  • domain assumption O-normal first-generation stars in globular clusters trace the oxygen abundance of their host galaxy at formation.
    Used to compute GC [O/Fe] from Carretta et al. (2010) and to use GCs as MW and GSE tracers (Sec. 3.3).
  • domain assumption Ar can act as a proxy for Fe and the Kobayashi et al. (2023) GCE conversion from O and Ar to [O/Fe] and [Fe/H] is valid for M31 planetary nebulae.
    Needed to place M31 PNe on the same scale as MW data; the conversion is model-based and from co-authors (Sec. 3.4, 5.2).
  • domain assumption At z~3 the MW was composed only of the inner halo and early high-alpha disc with no significant bulge component.
    Used to project the MW back to z~3 and assign mass (Sec. 6).
  • domain assumption The K20 GCE models describe the chemical evolution of the MW and GSE.
    Used for interpretation and for M31 conversion; models from Kobayashi et al. (2020a) and Kobayashi et al. (2023), co-authored by paper authors (Sec. 2.3).
  • domain assumption The McMillan (2017) potential and the Belokurov & Kravtsov (2023) E-Lz boundary correctly classify in-situ versus accreted stars.
    Underpins MW component definitions (Sec. 3.2.1).

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Cite this review

Pith. "Pith review of ChemZz I: Comparing Oxygen and Iron Abundance Patterns in the Milky Way, the Local Group and Cosmic Noon." pith.science (2026). https://pith.science/paper/ZMCUEJZL

@misc{pith2026250714094,
  author       = {Pith},
  title        = {Pith review of: ChemZz I: Comparing Oxygen and Iron Abundance Patterns in the Milky Way, the Local Group and Cosmic Noon},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/ZMCUEJZL}},
  note         = {Machine review of arXiv:2507.14094}
}
abstract

Our understanding of the chemical evolution of galaxies has advanced through measurements from both distant galaxies across redshift, and our own Milky Way (MW). To form a comprehensive picture, it is essential to unify these constraints, placing them on a common scale and parlance and to understand their systematic differences. In this study, we homogenize oxygen and iron measurements from star-forming galaxies at Cosmic Noon ($z{\sim}2-3$) with resolved stellar abundances from the Local Group. The MW is divided into four components, assuming the outer halo is dominated by debris from the Gaia-Sausage-Enceladus (GSE) progenitor. After converting all abundances to a common Solar scale, we identify clear $\alpha$- and iron-enhancement trends with mass in the $z{\sim}2-3$ galaxies and find good agreement between these galaxies and the MW high-$\alpha$ disc in [O/Fe] vs. [Fe/H]. We also find excellent agreement between the [O/Fe] trends seen in the MW high- and low-$\alpha$ discs with O-abundances seen in old and young planetary nebulae in M~31 respectively, supporting the existence of $\alpha$-bimodality in the inner regions of M~31. Finally, we use globular cluster ages to project the MW and GSE back in time to $z{\sim}3$ and find that their estimated mass, oxygen and iron abundances are strikingly consistent with the mass-metallicity relation of star-forming galaxies at $z{\sim}3$. In the future, increased transparency around the choice of Solar scale and abundance methodology will make combining chemical abundances easier -- contributing to a complete picture of the chemical evolution of all galaxies.

Figures

Figures reproduced from arXiv: 2507.14094 by the authors.

Figure 1
Figure 1. Representation of the “Tinsley-Wallerstein” diagram (Wallerstein 1962; Tinsley 1979), depicting the predicted chemical evolution of three dif￾ferent systems as a result of different star formation histories. Nucleosynthetic sources (driving the evolution) are marked, as well as the location of the “low- 𝛼” knee in the three systems. Predictions for the evolution of the MW bulge and high-𝛼 disc modeled by Kobayashi e… view at source ↗
Figure 2
Figure 2. The four MW components from our GALAH sample shown in both chemical and dynamical space. From left to right, the first column shows our definition for the four components in [𝛼/Fe] vs. [Fe/H] space. The three in-situ components are shown in black, while stars from the accreted halo are marked in cyan. Our chemical definition separating the high-𝛼 (thick) and low-𝛼 (thin) discs is marked in red, following the methodo… view at source ↗
Figure 3
Figure 3. Density contours of the four MW structural components we consider in [O/Fe] vs. [Fe/H] space using our cleaned GALAH catalogues after shifting into agreement with components in A19. Left, high resolution, 1D NLTE data for each component taken from the study of Amarsi et al. (2019) is over-plotted as the colour-coded points using their dynamical associations. The mean value of each component as a function of metallic… view at source ↗
Figures from the paper (4 more)
Figure 4
Figure 4. Figure 4: The specific star formation rates (sSFR ≡ SFR/𝑀∗) and stellar masses (M∗) for the Cosmic Noon samples at 𝑧 ∼ 2 (at a lookback time of ∼ 10.8 Gyr) and 𝑧 ∼ 3 (at a lookback time of ∼ 11.3 Gyr). Measurements from composite spectra reported by Steidel et al. (2016) and Cha…
Figure 5
Figure 5. Figure 5: The chemical evolution of the MW and four local dwarf galaxies in [O/Fe]K20 vs. [Fe/H]K20 is shown alongside the Cosmic Noon sample (coloured by mass) and data for the two PNe populations in M 31. The 𝑧 ∼ 2 Cosmic Noon sample is shown in the top row, while the 𝑧 ∼ 3 sa…
Figure 6
Figure 6. Figure 6: The chrono-chemical evolution of MW inner halo and high-𝛼 disc stars (black line in the left panel, rainbow line in the right panel), where the mean age is calculated for 0.2 dex bins in metallicity for both samples to determine the age gradient in the left panel. The …
Figure 7
Figure 7. Figure 7: Results of projecting the MW (primarily the inner halo or “Aurora”) and GSE to 𝑧 ∼ 3. Top, metallicity-mass relation (MZR) using 𝑍gas (oxygen abundance, red) and 𝑍∗ (iron abundance, blue) for the NIRVANDELS sample of individual galaxies (small points) and composites (l…

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