Gas-Phase Metallicity and Nitrogen Abundances in Low-Mass Galaxies Down to $M_\star\simeq10^{5.7}\,M_\odot$ at $z\simeq4.5$--$10.1$ from JWST Lensing Cluster Surveys

Hidenobu Yajima; Hiroya Umeda; Kimihiko Nakajima; Kuria Watanabe; Masami Ouchi; Moka Nishigaki; Ono Yoshiaki; Yi Xu; Yuichi Harikane; Yuki Isobe

REVIEW 4 major objections 8 minor 205 references

Gas-Phase Metallicity and Nitrogen Abundances in Low-Mass Galaxies Down to $M_\star\simeq10^{5.7}\,M_\odot$ at $z\simeq4.5$--$10.1$ from JWST Lensing Cluster Surveys

T0 review · 4 major / 8 minor · reviewed 2026-08-01 · deepseek-v4-flash

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Pith's one-line read Low-mass galaxies at z≈6 follow a steeper mass–metallicity relation than local galaxies, and their UV nitrogen lines reveal globular-cluster-like enrichment.

desk verdict Strong new JWST data extend the z~6 MZR to 10^6.6 Msun and show a stacked UV–optical N/O offset, but the steep low-mass slope relies on a Te scale that neglects O+3 and on a calibration fitted to the same stacks. read the letter →

arxiv 2607.15515 v1 pith:WB5I3B46 submitted 2026-07-17 astro-ph.GA

Hiroya Umeda , Masami Ouchi , Kimihiko Nakajima , Kuria Watanabe , Yuichi Harikane , Yuki Isobe , Moka Nishigaki , Ono Yoshiaki

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Hidenobu Yajima Yi Xu

This is my paper · ORCID

classification astro-ph.GA

keywords mass–metallicityrelationgas-phasemetallicitynitrogenabundancehigh-redshiftgalaxiesgravitationallensingstackedspectraWolf–Rayetstarsglobularclusters

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 uses 405 deep JWST spectra of gravitationally lensed galaxies at z=4.5–10.1, reaching stellar masses as low as 10^5.7 solar masses, to ask how metals accumulate in the smallest galaxies of the early universe. By stacking spectra in stellar-mass bins and detecting the faint [O III] 4363 auroral line down to a representative mass of about 10^6.6 solar masses, the authors build new empirical strong-line metallicity calibrations and trace the z~6 mass–metallicity relation down to 12 + log(O/H) ≈ 7.2. They find a low-mass slope of 0.38 ± 0.06, steeper than the local value of about 0.28, consistent with efficient metal loss or dilution in shallow gravitational potentials. In the combined stack, the nitrogen abundance inferred from the ultraviolet N IV] doublet exceeds the optical [N II]-based value by about 1.4 dex; together with strong He II 4686 emission, this points to a localized, highly ionized nitrogen-rich component—possibly Wolf–Rayet stars—whose wind nitrogen budget matches the nitrogen excess locked in globular-cluster-like stellar populations.

What carries the argument

The central machinery is mass-binned stacking of roughly 100 medium-resolution spectra (and about 400 at low resolution), which brings faint diagnostic lines above detection threshold. Metallicities come from the direct method using the [O III] 4363 auroral line under a two-zone ionization model with a fixed relation between low- and high-ionization electron temperatures; the authors then calibrate the R3 ([O III] 5007/Hβ) and R2 ([O II] 3727/Hβ) strong-line ratios against these direct metallicities to extend measurements to galaxies without auroral detections. The mass–metallicity relation is fitted with a turnover function. Nitrogen is measured twice: from the high-ionization UV doublet N

What would settle it

Measure [O III] 88 µm together with [O III] 5007 in a magnified galaxy with stellar mass near 10^6.6 solar masses at z~6: the far-infrared line gives an independent electron temperature and oxygen abundance. A value of 12 + log(O/H) more than about 0.3 dex above 7.2 at that mass would flatten the low-mass slope. Alternatively, a single high-signal-to-noise spectrum with auroral-line temperatures from both [O III] 4363 and [O II] 7325 that disagrees with the assumed two-zone temperature relation would force recalibration.

Watch

Extended reading notes

Core claim

The central discovery is that chemical enrichment in the lowest-mass high-redshift galaxies is both globally ordered and locally diverse. On the global scale, the gas-phase oxygen abundance falls steeply with stellar mass, with a fitted low-mass slope γ = 0.38 ± 0.06 that is steeper than the local relation; the relation reaches 12 + log(O/H) ≈ 7.2 at about 10^6.6 solar masses and matches a range of hydrodynamical simulations. On the local scale, the stacked spectrum at about 10^7.7 solar masses shows N/O from N IV] λλ1483,1486 that is about 1.4 dex higher than N/O from [N II] λ6583, with subsolar C/O and He II 4686/Hβ ≈ 0.03. The authors interpret this as a multi-zone interstellar medium in

Load-bearing premise

The entire metallicity scale rests on direct-method oxygen abundances that assume a two-zone ionization structure with a fixed electron-temperature relation (low-ionization temperature = 0.7 times high-ionization temperature plus 3,000 K) and neglect O+3; if this temperature or ionization prescription is biased, the calibrations, the mass–metallicity slope, and the N/O comparison all shift together.

Editorial extensions

If this is right

If the steep slope holds, the smallest galaxies at z~6 lose or dilute most of their metals, so their interstellar oxygen abundances sit roughly ten times below local galaxies of the same mass.
The new empirical strong-line calibrations can be applied to faint JWST samples without auroral lines, extending metallicity measurements to mass regimes that are otherwise inaccessible.
The systematic disagreement between UV and optical nitrogen diagnostics in the same systems means abundance interpretations based on only one spectral window are incomplete; each window traces a different gas phase.
Nitrogen overabundance seen in bright individual galaxies is also present in stacked low-mass populations, making it a common enrichment mode rather than a rare anomaly.
The comparable nitrogen mass in stellar winds and in globular-cluster enriched populations points to a concrete channel by which early, compact star formation could seed the abundance patterns seen in ancient star clusters.

Reading between the lines

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

If the multi-zone reading is right, single-zone N/O values in the literature that rely on UV lines alone are likely biased high by bright, N-rich clumps; correcting for this could bring many high-redshift nitrogen emitters back onto the local N/O–O/H sequence.
The same stacks could test the Wolf–Rayet hypothesis directly: medium-resolution spectroscopy of individual magnified clumps in z~6 lensed arcs should show whether N IV] and He II peak on globular-cluster-scale regions while [N II] traces the surrounding diffuse gas.
A prediction of the enrichment-burst picture is that metallicity and N/O should vary stochastically with star-formation history; comparing these stacks with simulations that track 10-million-year bursts could discriminate prompt Wolf–Rayet enrichment from delayed AGB winds.
The empirical calibration approach could be extended to C/O and Ne/O as functions of stellar mass, giving a two-element clock for the onset of enrichment in the lowest-mass galaxies.

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Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

First, the essential take: this paper brings genuinely new data to the table—405 lensed JWST/NIRSpec spectra reaching M*~10^6.6 Msun, the first direct-method metallicity at that mass, and a stacked detection of Niv]-based N/O higher than optical [Nii]-based N/O by 1.4 dex. That is worth having. But the headline slope of the MZR (γ=0.38±0.06) is not secure. It depends on direct-method oxygen abundances that assume a two-zone Te model and explicitly neglect O+3, and the lowest-mass bin (GM1) rests on a ~3σ [OIII]4363 detection.

What the paper does well: the stacking methodology is careful; AGN/LRD exclusion is thorough; the authors flag the GM4 data problems and the poorly constrained β. The N/O discrepancy is robust in the sense that even with the ~3σ Niv] line, the 1.4 dex offset is large. They test several alternative explanations (stack mixing, AGN-like radiation, density-bounded geometry) and honestly concede that the WR/GC connection is qualitative.

The soft spots, in order: (1) The empirical calibration is fitted to the same stacked spectra that are then used to derive the empirical MZR. So Fig. 10's agreement is not an independent validation; it's a tautology. This is acknowledged but should be presented clearly. (2) The O+3 neglect is more serious than a footnote. The paper's own HeII/Hβ≈0.03 and high O32 at low mass indicate hard radiation; in that regime O+3 can be a non-negligible fraction of oxygen. The bias would be larger at low mass, which would act to steepen the fitted slope. A +0.1–0.2 dex correction at the low-mass end could bring γ down to the local value. The authors mention the approximation but do not quantify it. (3) The Niv]/[Nii] offset is interesting but the absolute N/O scale depends on the ionizing spectrum (BPASS vs AGN changes it by ~0.2 dex), and the WNE nitrogen budget is an order-of-magnitude estimate with several hand-adopted parameters.

Bottom line: this is a solid observational paper, not a flashy claim. It deserves a serious referee. A revision should quantify the O+3 effect on the MZR slope, or explicitly present the slope as tentative rather than definitive. The data will be used regardless, so I'd cite it for the measurements even if I'm skeptical of the steepening.

Referee Report

4 major / 8 minor

Summary. Umeda et al. analyze 405 JWST/NIRSpec spectra of gravitationally lensed star-forming galaxies at z=4.5–10.1 from the DREAMS, GLIMPSE-D, GLASS, ERO, SPURS, UNCOVER, and CANUCS programs, with 50% of the M_UV>−17.5 sources magnified by μ>3. They construct stellar-mass-binned stacks (GM1–GM4, GAll and prism-resolution analogs), detect [OIII]λ4363 down to a representative stellar mass of ~10^6.6 M⊙, and derive direct-method oxygen abundances using a two-zone Te scheme (Eqs. 3–4). They fit new empirical R3/R2 strong-line calibrations (§4.4.2) to the direct-method stack metallicities, individual auroral-line detections, and local analogs, then apply them to trace the z~6 MZR to M*≈10^6.6 M⊙, fitting a Zahid et al. (2014) form with low-mass slope γ=0.38±0.06 (Table 6), reported as slightly steeper than the local γ≈0.28. In the GAll stack (M*≈10^7.7), the Niv]-based [N/O] is 0.66±0.24, ~1.4 dex above the [Nii]-based value (−0.73±0.11); with subsolar C/O and HeII λ4686/Hβ≈0.03, this is interpreted as a multi-zone ISM containing a localized, N-rich, globular-cluster-like component, with an order-of-magnitude estimate suggesting that a WNE-like stellar population could supply the required nitrogen mass.

Significance. The compiled lensing sample and the stacking products are a valuable community resource: the MZR baseline is extended two decades below previous z~6 measurements, the [OIII]λ4363 detection at M*≈10^6.6 M⊙ is a technically demanding result, and the tabulated empirical (Table 6) and photoionization-model (Table 7) calibrations are directly usable. The UV–optical N/O comparison in an average low-mass galaxy, if secure, would strengthen the case that nitrogen enhancement is widespread at high redshift and connect early enrichment to globular-cluster abundance patterns. These strengths are real, but the headline claims are currently anchored on a partly circular calibration, an unquantified O+3 systematic on the Te scale, and ~3σ line detections. The good news is that each of these can be quantified or tested with the authors' own model grids and robustness fits; the manuscript does not currently do so.

major comments (4)

[§4.4.2, §4.5, Eq. (7), Fig. 10] The new R3/R2 calibration is fitted using the direct-method metallicities of the same GM1–GM4 grating stacks (plus individual auroral-line detections and Andrews & Martini 2013 analogs) that are then used to construct the empirical MZR. The agreement between the direct and empirical methods shown in Fig. 10 is therefore partly by construction for the stacks, and the claim in §4.4.2 that this agreement 'demonstrates the internal consistency of the calibration' overstates the validation. The empirical MZR does not independently confirm the direct-method MZR; both trace the same Te-scale anchors. Please report the stack residuals in the calibration fit and perform a leave-one-stack-out cross-validation, so the reader can see how well the calibration predicts a stack excluded from the fit.
[§4.4.1, Eq. (4), Table 4, §5.1] Eq. (4) sums only O+ and O+2, and the paper notes (end of §4.4.1) that neglecting O+3 'may introduce a systematic uncertainty for systems with hard ionizing spectra' — exactly the regime probed here: HeII λ4686/Hβ≈0.03 (Table 3) and O32≳15 in GM1, decreasing to ≈4 in GM4 (Table 4). If a non-negligible O+3 fraction is present in the low-mass stacks, the direct-method O/H values are underestimated; because O32 is strongly mass-dependent, the bias is mass-dependent and will tend to steepen the fitted low-mass slope γ=0.38±0.06. A +0.1–0.2 dex correction at the GM1–GM2 end would bring the slope to the local value within the quoted uncertainty; the current ~1.7σ difference from the local γ≈0.28 is not robust to this systematic. Please quantify O+3/O using the paper's own Cloudy model grids (Appendix A) at the observed O32, C43, and HeII strengths, and quote γ with and without the correction.
[Table 2, Table 4, §4.5] The two lowest-mass anchors are fragile. (i) GM1's [OIII]λ4363/Hβ=0.12±0.04 is a ~3σ detection, at the adopted stack threshold; its direct-method oxygen abundance (12+log(O/H)=7.27^{+0.21}_{-0.14}) carries this statistical fragility into the MZR fit. (ii) GM1's [OII] is a 3σ upper limit (<0.21), so R2 is not measured, yet the quoted empirical metallicity uncertainty for GM1 (7.27±0.06) is smaller than the direct-method uncertainty and it is unclear how the upper limit enters the likelihood of Eq. (6). Because GM1 is the point that controls the difference between γ=0.38 and the local γ≈0.28, the paper should show the MZR refit with GM1 excluded and state explicitly how upper limits are propagated in Eq. (6).
[§4.6.1, Table 3, Appendix A] The claimed 1.4-dex discrepancy between [N/O]UV=0.66±0.24 and [N/O]Opt=−0.73±0.11 rests on the Niv] λλ1483,1486 detection in GAll at S/N≈3 (flux 0.12±0.05; the stack detection criterion is S/N≥3), and on a photoionization-model ionization correction whose AGN variant shifts the Niv]/Oiii] calibration by ≈0.2 dex (Table 7). Please report the achieved S/N of Niv] explicitly, propagate the spread among the stellar, AGN, and WNE calibrations (Table 7) into [N/O]UV, and state how the significance of the 1.4-dex offset is affected once this model systematic is included. As written, the statistical and model uncertainty budget is not sufficient to establish the discrepancy quantitatively, even though the direction of the offset is consistent with literature results.

minor comments (8)

[§4.2, Table 6] The fitted O32 relation is printed as logO32 = −0.243±0.004 + (2.89±0.27) log(M⋆/M⊙). As written this has the wrong sign/roles: it predicts O32 increasing steeply with stellar mass, contradicting the text ('higher ionization parameter at lower stellar mass') and Fig. 7; the intended relation is logO32 ≈ 2.89 − 0.24 log(M⋆/M⊙) (with the coefficients interchanged and b1 negative). Since this relation is used to infer R2 in Eq. (6), the printed formula must be corrected for reproducibility.
[Table 4] The O32 column lists linear ratio values (e.g., 12.86^{+2.17}_{-1.47} for GM2 and the lower limit >15.01 for GM1) while §4.2 and Fig. 7 work in log space. Please state units in the column header and mark GM1's entry explicitly as a lower limit throughout (as done in Table 2 for [OII]).
[§4.5, Table 6] The MZR is fit to four stack points with three effective free parameters (β fixed at 49). Report the covariance among Z0, logM0, and γ, and add the 0.07–0.08 dex RMS of the strong-line calibration (Table 6) and Te-scale systematics to the quoted γ uncertainty. The abstract's 'slightly steeper' is appropriately cautious, but Summary item 2 ('steep low-mass-end slope... sharp decrease') is stronger than justified by a ~1.7σ difference from the local γ≈0.28.
[§2.5–§4.5] The sample spans z=4.5–10.1 and the MZR is labelled z~6. Please state the median redshift of each stack (GM1–GM4, GAll) to quantify the epoch over which each stack is averaged; a ~1-Gyr baseline could introduce redshift-evolution scatter into the stacked MZR.
[Tables 2–3] Please report the achieved S/N for the marginal detections ([OIII]λ4363 in GM1, Niv] in GAll, [NII]λ6583 in GAll) in the tables, since the stacked criterion is S/N≥3 and several values sit at or near this boundary.
[§2.1.1] The DREAMS data reduction is described as 'forthcoming (Nakajima et al., in preparation)'. For reproducibility, cite the public data products or the companion pipeline paper, and provide the same for the other survey reductions where available.
[Throughout] Typographical issues: 'T able' (Table 1 caption); 'W AIC'/'∆W AIC' (§2.3); inconsistent 'Wolf-Rayet' vs 'Wolf–Rayet'; 'Hβflux' missing space (§3); corrupted symbol 'λW4686' in the abstract; 'D WN' in the Acknowledgments; 'MAG AUTO' should be MAG_AUTO; mass-loss units 'M⊙ yr−1' are missing after Ṁ in §5.3.
[Introduction, References] The Introduction cites 'A. J. Cameron et al. 2023' for high-z nitrogen enhancement; the widely used reference for a nitrogen-enhanced galaxy at z~5–7 is Cameron et al. 2024 (Nature). Please verify the intended citation and that the reference list entries ('Cameron et al. 2023' and 'Cameron et al. 2026') correspond to the claimed results.

Circularity Check

1 steps flagged · score 5.0 of 10

The empirical-calibration MZR for the stacks re-states the same direct-method O/H values the calibration was fitted to; the steep low-mass slope is not an independent strong-line prediction, though the direct-method MZR gives some independent support.

fitted input called prediction [Section 4.4.2 (Strong-Line Calibrations), Section 4.5 (Mass–Metallicity Relation), Eq. (7), Table 6, Figs. 9–10]
"Instead of adopting a calibration from the literature, we derive empirical relations between the strong-line ratios and direct-method metallicity ... The fit uses our grating stacked spectra and individual measurements with auroral-line detections. ... Based on the newly derived calibration, we derive strong-line based empirically calibrated metallicities ... for individual galaxies and stacked spectra using the observed R3 and R2 values. ... We fit the MZR using the stacked spectra metallicity measurements based on the empirical calibration."

The R2/R3 calibration is fitted to direct-method 12+log(O/H) values of the same grating stacks (GM1–GM3) and individual galaxies with [OIII]4363 detections. Those same stacks are then assigned 12+log(O/H)_Emp by inverting that calibration, so their empirical metallicities coincide with the direct-method inputs to within the polynomial fit residuals (Fig. 10). Fitting the MZR (Eq. 7) to these empirical stack values therefore makes the resulting low-mass slope gamma=0.38+/-0.06 a smoothed re-statement of the direct Te-based O/H of the same bins, not an independent strong-line prediction. GM1 is additionally self-referential: [OII] is a non-detection, so R2 is imported from the O32–M* relation fitted on the same stacks, making the lowest-mass anchor twice dependent on its own direct-method va

full rationale

The identifiable circular step is confined to the empirical strong-line calibration pipeline. The paper explicitly fits the calibration to direct-method metallicities of the grating stacks and then uses the empirically calibrated metallicities of those same stacks to fit the MZR; for GM1–GM3 the empirical values are, by construction, close to the input direct-method values. Therefore the advertised 'empirical calibration' MZR for the stacks is not an independent confirmation of the direct-method result. The paper does, however, also present a direct-method MZR (Fig. 12) that is independent of the calibration itself, and the direct Te measurements are not derived from the strong-line calibration. So the steep low-mass slope is not wholly manufactured; it inherits whatever systematic biases are in the Te method (e.g., the assumed Te([OII])–Te([OIII]) relation and neglected O+3), which is a correctness/robustness concern rather than circularity per se. No load-bearing self-citation or uniqueness-imported-from-authors pattern was found; self-citations to Isobe, Nakajima, Ouchi, and other (partly overlapping) works are methodological and do not by themselves force the conclusions. Score 5 reflects one genuine partial circularity in the empirical-calibration MZR, with the central claim still retaining independent direct-method content.

Assumptions & free parameters 4 free parameters · 8 assumptions · 1 invented entities

The central measurements rest on standard JWST reduction and SED fitting, plus a newly derived strong-line calibration that is partly fitted to the same stacked spectra it calibrates; the N/O and WR/GC interpretation adds adopted stellar-atmosphere and globular-cluster parameters.

free parameters (4)

MZR fit parameters (Z0, logM0, gamma, beta) = Z0=8.06±0.09, log(M0/Msun)=8.85±0.31, gamma=0.38±0.06, beta=49
Fitted to stack metallicities in Eq. 7; beta poorly constrained and effectively fixed, so the low-mass slope is the main fitted quantity.
Strong-line calibration coefficients (c0,c1,c2 for logR3 and logR2) = logR3: 0.0680, 1.8282, -1.0690; logR2: -1.2276, 1.7359, -0.3747
Polynomial coefficients fitted to direct-method metallicities of grating stacks, individual auroral detections, and Andrews & Martini (2013) analogs.
Stellar-mass–line-ratio relations (logO32, logC43) = logO32 = -0.243 + 2.89 logM; logC43 = -0.60 + 4.33 logM
Used to infer R2 and C43 for sources without [OII] coverage and for abundance calibrations; fitted to the stacks.
WNE/GC mass-budget assumptions = N_WN~1650, t_WNE=0.5 Myr, X_N=1.5e-3, f_enriched=0.7, [N/H]_enriched=-0.7, M_GC=2e5 Msun
Hand-adopted values in the order-of-magnitude estimate linking HeII and nitrogen wind mass to globular-cluster excess.

assumptions (8)

domain assumption Te([OII]) = 0.7 Te([OIII]) + 3000 K
Empirical relation from Campbell/Garnett used for all direct-method O/H; §4.4.1.
domain assumption Two-zone ionization model neglecting O+3
O/H from O+ and O+2 only; O+3 contribution could bias metallicities; §4.4.1.
domain assumption Electron density adopted from Topping et al. (2025) redshift relation
Used for abundance calculations rather than per-stack measured densities; §4.3.
domain assumption BPASS v2.2.1 + Cloudy grids and Calzetti attenuation for SED fitting
Stellar masses and SFRs from Bagpipes; §2.4.
domain assumption Photoionization abundance calibrations assume plane-parallel, constant-density clouds with solar relative abundances
N/O, C/O, Ne/O, Ar/O inferred through offsets from solar-pattern model sequences; Appendix A.
domain assumption Lensing magnification models are correct
Absolute UV magnitudes and derived stellar masses depend on glafic/UNCOVER/CANUCS lens models; §2.2.
ad hoc to paper WNE parameters (logT*=5.25, Mdot=1.2e-5 Msun/yr, M*=12 Msun)
Adopted PoWR SMC WNE model used to estimate N_WN and nitrogen wind mass; §5.3.
ad hoc to paper Globular-cluster enrichment parameters (f_enriched=0.7, [N/H]_enriched=-0.7, M_GC=2e5 Msun)
Order-of-magnitude comparison of nitrogen mass; §5.3.

invented entities (1)

WNE-like stellar population component beyond BPASS
purpose: Explains HeII 4686/Hbeta~0.03 and the UV nitrogen excess with ~1650 WNE-like stars contributing ~10% of Hbeta
Phenomenological component introduced in §5.3; its existence is inferred from the same line ratios it is meant to explain, and the paper explicitly cautions it is not a simple addition of ordinary WR stars to BPASS.

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Cite this review

Pith. "Pith review of Gas-Phase Metallicity and Nitrogen Abundances in Low-Mass Galaxies Down to $M_\star\simeq10^{5.7}\,M_\odot$ at $z\simeq4.5$--$10.1$ from JWST Lensing Cluster Surveys." pith.science (2026). https://pith.science/paper/WB5I3B46

@misc{pith2026260715515,
  author       = {Pith},
  title        = {Pith review of: Gas-Phase Metallicity and Nitrogen Abundances in Low-Mass Galaxies Down to $M_\star\simeq10^5.7\,M_\odot$ at $z\simeq4.5$--$10.1$ from JWST Lensing Cluster Surveys},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/WB5I3B46}},
  note         = {Machine review of arXiv:2607.15515}
}

abstract

We analyze 405 deep JWST/NIRSpec spectra of star-forming galaxies at $z=4.5$--$10.1$ from DREAMS and other lensing-cluster surveys to study chemical enrichment in intrinsically faint, low-mass galaxies. The sample covers $M_{\rm UV}\simeq-12$ to $-22$ and reaches $M_\star\simeq10^{5.7}\,M_\odot$, with 50\% of the sources at $M_{\rm UV}>-17.5$ magnified by $\mu>3$. From individual spectra and mass-binned stacks, we derive the gas-phase metallicity together with nitrogen and carbon abundances using the rest-frame UV and optical lines. \Add{We derive new empirical strong-line metallicity calibrations using direct-method measurements from stellar-mass-binned stacks, reaching a representative stellar mass of $M_\star\simeq10^{6.6}\,M_\odot$. Applying these calibrations, we trace the $z\sim6$ mass--metallicity relation down to $M_\star\simeq10^{6.6}\,M_\odot$, where it reaches $12+\log({\rm O/H})\simeq7.2$, with a low-mass slope slightly steeper than the local relation and in broad agreement with hydrodynamical simulations.} In the $M_\star\simeq10^{7.7}\,M_\odot$ stack, N/O from N\,{\sc iv}]\,$\lambda\lambda\,1483,1486$ exceeds that from [N\,{\sc ii}]\,$\lambda6583$ by $\simeq1.4$ dex. The UV--optical difference could indicate a localized, highly ionized N-rich component whose high N/O and subsolar C/O resemble nitrogen-rich globular-cluster populations with $M_\star\lesssim10^6\,M_\odot$. \Add{The combination of these abundance patterns and a He\,{\sc ii}\,\W4686/H$\beta$ ratio of $\simeq0.03$, well above BPASS predictions, suggests that WR stars may contribute both prompt CNO-cycle enrichment and hard ionizing radiation, with the inferred WR population potentially supplying enough nitrogen to account for the excess on globular-cluster scales.

Figures

Figures reproduced from arXiv: 2607.15515 by the authors.

**Figure 1.** The distribution of UV magnitude by redshift for the sample after excluding AGN and LRD candidates. Circles and crosses correspond to the objects at z < 8 (z > 8) with F150W (F200W) band detection or non-detection, respectively. For the non-detection sources, we present the 3σ upper limit. The colors indicate the magnification factor, with the color bar at left showing the corresponding scale [PITH_FULL_IMAGE:fig… view at source ↗

**Figure 2.** The BPT diagram. The objects encircled by blue diamonds, red circles, and yellow pentagons represent the AGN candidate selected from the broad line detection (Type-I AGN candidate), BPT selection, and red optical slope (i.e., LRD candidates). 2.5.1. Sample Selection To mitigate AGN contamination, we exclude galaxies showing AGN-like line ratios using the classical BPT diagram based on [O iii]/Hβ and [N ii]/Hα where… view at source ↗

**Figure 3.** The stacked spectra of the full star-forming galaxy sample at grating (GAll) and prism (PAll) resolutions are shown in the top and bottom panels, respectively. For both the GAll and PAll spectra, the UV (left) and optical (right) components are arbitrarily normalized for visualization. The wavelengths of key emission lines are marked by vertical dotted lines. The shaded regions indicate the 1σ uncertainties estimate… view at source ↗

Figures from the paper (18 more)

**Figure 4.** Figure 4: Zoomed-in stacked spectra around key UV and optical emission lines, including C iv λλ1548,1551, C iii] λλ1907,1909, [O ii] λλ3727, 3729, Hγ+[O iii] λ4363, Hβ+[O iii] λλ4959, 5007, Hα, and [S ii] λλ6716,6731. The spectra are shown in the rest frame and are arbitrarily s…

**Figure 5.** Figure 5: Zoomed-in GAll stacked spectra around key optical and UV emission lines. The left panel shows the UV spectra around N iv] λλ1483, 1486, C iv λλ1548, 1551, He ii λ1640 + O iii] λλ1661, 1666, the N iii] λ1750 quintet, Si iii] λλ1883, 1892, and C iii] λλ1907, 1909. The r…

**Figure 7.** Figure 7: Stellar-mass dependence of (a) O32 and (b) C43. In panel (a), the solid black dots represent individual galaxies with detections of [O ii] λλ3726, 3729 and [O iii] λλ4959, 5007, while the transparent black dots represent galaxies with non-detections of [O ii] λλ3726,…

**Figure 8.** Figure 8: Electron density inferred from the [S ii] λλ6716,6731 and C iii] λλ1907,1909. The turquoise and orange symbols represent the electron density measurements based on the [S ii] and C iii] ratios as a function of stellar mass, respectively. The squares and stars represent…

**Figure 9.** Figure 9: Empirical calibrations between strong-line ratios and direct-method metallicity. (a) The relation between R3 and 12 + log(O/H). (b) The relation between R2 and 12 + log(O/H). The red squares and black circles represent measurements from our grating stacked spectra and …

**Figure 10.** Figure 10: The comparison between the gas-phase metallicities measured from the direct method and the empirical strong line relations. The black dots represent the measurements for the grating galaxy spectra with [O ii] λλ3726, 3729, [O iii] λ4363, Hβ, and [O iii] λλ4959, 5007…

**Figure 11.** Figure 11: The stellar-mass and gas-phase metallicity relation (MZR) at z ∼ 6 (i.e., z ≃ 4.5 − 9) based on the strong line calibrations. The black circles represent the measurement from individual galaxies with Hβ or [O iii] λλ4959,5007 detections. The large red squares represen…

**Figure 14.** Figure 14 [PITH_FULL_IMAGE:figures/full_fig_p019_14.png]

**Figure 13.** Figure 13: The comparison between the MZR measurement based on the R ∼ 1000 stacked spectra (red circles), R ∼ 100 stacked spectra (turquoise squares), and the binned measurements from individual galaxies (grey diamonds). the physical assumptions and the other observables such …

**Figure 15.** Figure 15: (a) The [N/O] abundance ratio derived using N iv] λλ1483,1486 and O iii] λλ1661,1666 as a function of stellar mass. The red star represents our measurement for the GAll stack. The grey, blue, and red symbols correspond to the measurements for z ∼ 0 (Z. Martinez et al.…

**Figure 16.** Figure 16: (a) The [N/O] abundance ratio derived using N iv] λλ1483,1486 and O iii] λλ1661,1666 as a function of gas-phase metallicity. The red star represents the our measurement for GAll stack. The grey, blue, and red symbols correspond to the measurements for z ∼ 0 (Z. Martin…

**Figure 17.** Figure 17: (a) The [C/O] abundance ratio derived using UV spectra as a function of stellar mass. We show the measurements of the z ∼ 2 galaxies from D. A. Berg et al. (2019) in grey diamonds and the literature z > 6 N-enhanced galaxies in red diamonds (e.g., Y. Isobe et al. 2023…

**Figure 18.** Figure 18: The mass–metallicity relation from the simulations with different ISM assumptions. The blue solid, orange dashed, purple dotted, and yellow dotted-dahsed lines represent the mass–metallicity relation predictions by the Fire-2 (A. Marszewski et al. 2024), FirstLight …

**Figure 19.** Figure 19: The [C/O]UV vs. [N/O]UV abundance ratio. The red star represents the measurements for the stacked spectra from all galaxy grating spectra. The other red symbols represent the abundance measurements of N iv] emitters from literature. The gray solid line corresponds to …

**Figure 20.** Figure 20: (Top): The [N/O] vs. [Ar/O] and [N/O] vs. [Ne/O] abundance ratios. (Bottom): The [C/O] vs. [Ar/O] and [C/O] vs. [Ne/O] abundance ratios. For GAll, Ar/O is a 1σ upper limit, indicated by the leftward arrows, whereas Ne/O is a measurement. The symbols are otherwise the …

**Figure 21.** Figure 21: Comparison of the observed He ii λ4686/Hβ ratio with the maximum values predicted by the BPASS, AGN, and WNE models as a function of C43. The observed value is shown by the yellow star, while the shaded regions extending up to the model maxima represent BPASS (black…

**Figure 22.** Figure 22: The [N/O] abundance ratio as a function of (a) stellar mass and (b) gas-phase metallicity. The red and gray symbols represent UV- and optical-based N/O measurements, respectively, from this work and the literature samples compiled in Figures 15 and 16. The red and gra…

**Figure 23.** Figure 23: Photoionization-model relations between C iv/C iii] and the abundance-sensitive N iv]/O iii], C iii]/O iii], [Ar iv]/O iii], and [Ne iii]/O iii] emission-line ratios. All models use a plane-parallel, constant-density cloud with solar relative abundances and span −3 ≤…

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Pith tools

Reviewed August 1, 2026 · model on record in the stance chip above.

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