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The JWST EXCELS survey: direct estimates of C, N, and O abundances in two relatively metal-rich galaxies at $\mathbf{z\simeq5}$

T0 review · 2 major / 4 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read Direct JWST measurements in two $z\simeq5$ galaxies find nitrogen enrichment outpacing carbon, suggesting early galaxies favour N over C even at moderate metallicity.

desk verdict Two careful new direct CNO abundance points at z~5 in a metal-rich regime, with the main caveat being the zero-reddening assumption that the paper itself honestly quantifies. read the letter →

arxiv 2412.10557 v2 pith:XEYKSJXW submitted 2024-12-13 astro-ph.GA

K. Z. Arellano-Córdova , F. Cullen , A. C. Carnall , D. Scholte , T. M. Stanton , C. Kobayashi , Z. Martinez , D. A. Berg
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L. Barrufet R. Begley C. T. Donnan J. S. Dunlop M. L. Hamadouche D. J. McLeod R. J. McLure K. Rowlands A. E. Shapley
This is my paper · ORCID
classification astro-ph.GA
keywords galaxyabundanceschemicalevolutionhigh-redshiftgalaxiesJWSTNIRSpecdirectmethodC/NabundanceratiosN/Oenrichmentinitialmassfunction
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper reports the first direct, temperature-based measurements of carbon, nitrogen, and oxygen in two relatively metal-rich star-forming galaxies at $z\simeq5$, from JWST/NIRSpec spectra. Both galaxies show elevated N/O and low C/O relative to typical local galaxies, so their C/N ratios sit below the local sequence at fixed O/H. The authors argue that this 'nitrogen over carbon' pattern, previously seen in metal-poor galaxies at $z>6$, extends to moderate metallicities of roughly $0.2\!-\!0.3$ solar, and that it is best explained by carbon from core-collapse supernovae together with delayed nitrogen from intermediate-mass AGB stars. If correct, the result means early-Universe enrichment is not only a feature of the most primitive galaxies, and it shows that JWST can deliver robust direct CNO abundances at $z\sim5$.

What carries the argument

The direct, temperature-sensitive abundance method: the [O III] $\lambda4363/\lambda5007$ ratio fixes the electron temperature, C III] $\lambda\lambda1906,09$ gives $\mathrm{C}^{2+}$, [O II] $\lambda\lambda3726,29$ and [N II] $\lambda6584$ give $\mathrm{O}^{+}$ and $\mathrm{N}^{+}$, and ionisation correction factors convert ionic to total abundances. The resulting C/N versus O/H diagram is interpreted with the chemical evolution models adopted in the paper for different IMF slopes. The load-bearing mechanism is the relative timing of enrichment: massive stars release C and O promptly at core collapse, while intermediate-mass AGB stars add N later, so low C/N at fixed O/H tracks delayed or enhanced nitrogen relative to carbon.

What would settle it

A high-signal-to-noise Balmer decrement (or a Paschen-to-Balmer ratio) for a larger sample of $z\simeq5$ NIRSpec galaxies that unambiguously returns $E(B-V)\gtrsim0.1$ would falsify the zero-reddening assumption and shift the inferred C/N ratios toward the local sequence. Alternatively, a stacked spectrum of many $z\simeq5$ galaxies with [O III] $\lambda4363$, C III], and [N II] that shows the same low C/N at fixed O/H after a robust reddening correction would confirm the claim.

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Extended reading notes

Core claim

Using the [O III] $\lambda4363$ auroral line to fix the electron temperature, the paper derives oxygen abundances of $12+\log(\mathrm{O/H})=8.21^{+0.08}_{-0.05}$ and $7.97^{+0.05}_{-0.04}$, nitrogen ratios of $\log(\mathrm{N/O})=-1.07^{+0.17}_{-0.13}$ and $-0.86^{+0.15}_{-0.11}$, and carbon ratios of $\log(\mathrm{C/O})=-0.82\pm0.22$ and $-1.02\pm0.22$ in EXCELS-70864 and EXCELS-121806. These values put the galaxies on the local mass--metallicity relation but in the high-metallicity tail of the direct-method $z\gtrsim5$ sample. At fixed O/H their N/O is high and C/O low compared with most $z\sim0$ galaxies, and the paper concludes that the resulting low C/N ratios indicate a preferential enrichment of nitrogen over carbon in the ISM at $z>5$, with carbon from core-collapse supernovae and nitrogen from roughly $4\!-\!7\,M_\odot$ intermediate-mass stars. Comparison with chemical evolution models favours a steeper, bottom-heavy IMF over a standard IMF, although a standard IMF is not ruled out.

Load-bearing premise

The analysis assumes the two galaxies have no dust reddening ($E(B-V)=0$) because their Balmer line ratios agree with the dust-free Case B values only within $2\sigma$; if a small reddening such as $E(B-V)\simeq0.15$ is real, the derived C/N ratios would rise toward the local values and the paper's central offset would weaken.

Editorial extensions

If this is right

  • The nitrogen-over-carbon offset found in metal-poor $z>6$ galaxies also appears at $Z\simeq0.2\!-\!0.3\,Z_\odot$ at $z\simeq5$, so the pattern is not confined to the most primitive systems.
  • At these metallicities the inferred enrichment channels are carbon from core-collapse supernovae and nitrogen from intermediate-mass ($\simeq4\!-\!7\,M_\odot$) AGB stars, which predicts a delayed N build-up after each burst.
  • Chemical evolution models with a steeper, bottom-heavy IMF reproduce the observed C/N better than the standard Kroupa IMF, although the standard IMF remains consistent within the uncertainties.
  • These are among the first direct-method C, N, and O measurements at $z\gtrsim5$, roughly doubling the small existing sample, so larger JWST programs at $z=4\!-\!7$ can test the trend.
  • The two galaxies sit on the local star-forming main sequence and mass--metallicity relation, so their unusual CNO patterns are not explained by unusual global properties.

Reading between the lines

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

  • If the offset holds in a larger sample, C/N at fixed O/H could become an empirical clock for the time since the last starburst, because nitrogen from intermediate-mass stars appears later than carbon and oxygen from core collapse; this is an editorial inference beyond the paper's claims.
  • The similarity between these $z\sim5$ abundances and local Lyman-continuum leakers hints that low C/N gas may accompany ionising-photon escape, a connection the paper notes only in passing; tracking C/N against measured escape fractions would test it.
  • A bottom-heavy IMF, if real, would change stellar-mass-to-light ratios and could bias SED-based stellar masses toward higher values than Kroupa-IMF fits; comparing dynamical masses with SED masses for these galaxies would be a testable consequence.
  • The zero-reddening assumption is the main systematic: a modest $E(B-V)\simeq0.15$ would move the C/N ratios toward the local relation, so higher signal-to-noise Balmer decrements in these two objects would directly decide between dust and genuine enrichment.
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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

2 major / 4 minor

Summary. The paper presents JWST/NIRSpec medium-resolution spectroscopy of two z≈5 star-forming galaxies from the EXCELS survey, with detections of [O III] 4363, C III] λλ1906,09, [O II] λλ3726,29, and [N II] 6584. The authors derive direct, temperature-sensitive abundances: 12+log(O/H) = 8.21(+0.08/−0.05) and 7.97(+0.05/−0.04), log(N/O) = −1.07(+0.17/−0.13) and −0.86(+0.15/−0.11), and log(C/O) = −0.82±0.22 and −1.02±0.22. They compare these values with local and high-redshift samples and argue that the C/N versus O/H diagram shows a systematic preference for N over C enrichment at z≳5, possibly extending to relatively metal-rich, evolved systems; a comparison with Kobayashi et al. (2020) chemical evolution models is used to suggest that a standard or bottom-heavy IMF can reproduce the observed patterns. The paper includes Monte Carlo uncertainty propagation, a UV/optical temperature cross-check for one object, and an explicit discussion of the dust vector in the C/N plane.

Significance. If the abundance measurements are robust, this paper would add the first direct CNO abundance determinations at z≈5 in relatively metal-rich galaxies, increasing the small sample of direct-method z≳5 CNO measurements by 50% and providing a new constraint on enrichment timescales and the IMF at early epochs. The analysis is careful in several respects: the [O III] 4363 auroral line is detected in both targets, the line-flux uncertainties include an empirically estimated excess scatter, and the authors explicitly show the effect of E(B−V)=0.15 on their central ratio. These strengths make the paper a valuable observational contribution even if some of the interpretive claims are provisional.

major comments (2)
  1. [§3.2, Fig. 3, Table 2] The statement that all Balmer ratios are consistent with Case B within 2σ is not supported by the listed fluxes. For EXCELS-70864, Hα/Hβ using the G235M Hβ measurement is 64.13/28.26 = 2.27, which is ≈5.7σ below the Case B value of 2.78 using only the quoted statistical uncertainties; even adding the stated 8% cross-grating calibration uncertainty in quadrature leaves a discrepancy of ≈2.5σ. The adoption of E(B−V)=0 therefore rests on a weaker empirical basis than claimed, and the independent Hγ/Hβ and Hδ/Hβ estimates (E(B−V)=0.19±0.11 and 0.13±0.08) are not consistency proofs for zero reddening but rather additional indicators that the reddening assumption is the dominant systematic in this analysis.
  2. [§4.5 and Fig. 7] The central claim of preferential N over C enrichment is not robust to modest nebular reddening. The paper itself shows that E(B−V)=0.15 shifts log(C/N) by an amount comparable to the separation between the high-redshift and local samples, moving the EXCELS points toward the local relation, and the authors' own higher-order Balmer estimates are of this order. Because CIII] 1909 and [NII] 6584 are separated by ~4500 Å in the rest frame, any differential reddening directly changes the derived C/N, and the claimed bottom-heavy IMF preference is based on the zero-reddening values. The manuscript needs either a quantitative propagation of the E(B−V)=0.15–0.2 systematic into the reported abundance ratios and the model comparison, or an explicit demonstration that the zero-reddening assumption is not responsible for the observed C/N offset.
minor comments (4)
  1. [Table 1] The final row lists the galaxy as EXCELS-70684, but the galaxy is EXCELS-70864 elsewhere in the paper; this typo should be corrected.
  2. [§3.4.1] The text refers to 'EXCELS-70868' when deriving the electron temperature; the intended object is EXCELS-70864.
  3. [Fig. 2 caption] The caption states that EXCELS-121806 is at z=5.255, but the redshift given in the text and Table 1 is 5.225.
  4. [§3.4.2] The sentence 'we have added in quadrature an uncertainty of 610 K and 1300 K' should read '±610 K and ±1300 K' to make the intended values clear.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the C, N, O abundances are measured from line fluxes with independent atomic data and published ICFs, and the model comparison is explicitly illustrative rather than fitted.

full rationale

The derivation chain is self-contained: emission-line fluxes are measured from the spectra (Sec. 3.1), electron temperatures and densities come from [O III] and [S II] ratios with PyNeb atomic data (Sec. 3.4.1), and total abundances are obtained from ionic abundances plus published ICFs (Sec. 3.4.2). The C/N, C/O, and N/O values do not reduce to any fitted parameter or to the chemical evolution models. In Sec. 4.5.1 the authors state that they are 'not attempting to find an exact match' and later call the model comparison 'purely illustrative', so the IMF discussion does not define or generate the measured ratios. The zero-reddening assumption in Sec. 3.2 is a physically motivated systematic assumption, and the paper explicitly flags it in Sec. 4.5 with the dust vector in Fig. 7; this is a caveat, not a circular reduction. Local comparison values from in-preparation papers by group members are comparison anchors, not inputs to the abundance derivation, and the central measurements remain independent of those anchors. There is no self-citation chain that forces the claimed result, no fitted input renamed as a prediction, and no uniqueness theorem imported from the authors.

Assumptions & free parameters 5 free parameters · 6 assumptions · 0 invented entities

The central abundance estimates rest on standard nebular analysis with several adopted physical conditions, including zero reddening, an assumed density, inferred temperatures, and published ionization correction factors. The model interpretation introduces toy SFH and IMF slopes rather than fitting the data. No new particles, forces, or physical entities are postulated.

free parameters (5)
  • Nebular reddening E(B-V) = 0
    Assumed from Balmer decrements; Halpha/Hbeta lies below Case B but within 2 sigma of zero reddening. A nonzero value would raise C/N, as shown in Fig. 7.
  • Electron density n_e = 600 cm^-3, adopted for EXCELS-70864 from EXCELS-121806
    Only EXCELS-121806 constrains n_e via [S II]; the same value is assumed for EXCELS-70864. N/O shifts by 0.33 dex at n_e=10^4 cm^-3.
  • T_e[O II] = From Arellano-Cordova and Rodriguez (2020) relation
    The low-ionization zone temperature is not measured and is estimated from an empirical relation that depends on ionization parameter.
  • T_e[S III] = From Garnett (1992) photoionization models
    The intermediate-ionization zone temperature is not measured and is used for C2+ and Ar2+.
  • Chemical evolution model IMF slope x = x = 1.1, 1.3, 1.9, 2.3
    Illustrative models vary IMF slope and toy star-formation history timescales to interpret C/N; these are not fitted to the data.
assumptions (6)
  • domain assumption Case B recombination Balmer ratios at Te=15,000 K and ne=300 cm^-3
    Used to assess reddening; if the nebula is density-bounded or departs from Case B, the zero-reddening assumption fails (Section 3.2).
  • standard math Five-level atom atomic data and PyNeb collision strengths
    Standard nebular analysis; adopted atomic data are listed in Section 3.4.1.
  • domain assumption Ionization correction factors: N/O = N+/O+, C ICF from Berg et al. (2022), Ne ICF from Dors et al. (2013), Ar ICF from Izotov et al. (2006)
    Unseen ionization stages are corrected with published factors; differences are small for C but not fully verified for these objects (Section 3.4.2).
  • domain assumption Star formation is the only ionization source
    AGN is ruled out only by BPT proximity and lack of broad lines; shocks or AGN would invalidate the abundance derivation (Section 3.3).
  • domain assumption Kobayashi et al. (2020) chemical evolution yields and IMF prescriptions
    The model comparison in Section 4.5.1 assumes these yields and a toy SFH; results are illustrative and depend on a coauthor's model grid.
  • domain assumption Literature abundances from original papers are directly comparable without recalculation
    The comparison sample uses heterogeneous Te relations, atomic data, and ICFs; the paper notes this and does not homogenize (Section 2.2).

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Cite this review

Pith. "Pith review of The JWST EXCELS survey: direct estimates of C, N, and O abundances in two relatively metal-rich galaxies at $\mathbf{z\simeq5}$." pith.science (2026). https://pith.science/paper/XEYKSJXW

@misc{pith2026241210557,
  author       = {Pith},
  title        = {Pith review of: The JWST EXCELS survey: direct estimates of C, N, and O abundances in two relatively metal-rich galaxies at $\mathbfz\simeq5$},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/XEYKSJXW}},
  note         = {Machine review of arXiv:2412.10557}
}
abstract

We present a spectroscopic analysis of two star-forming galaxies at $z\simeq5$ observed with JWST/NIRSpec as part of the EXCELS survey. The detection of the CIII]~$\lambda\lambda$1906,09, [OII] $\lambda\lambda$3726,29, [OIII] $\lambda\lambda$4363,5007, and [NII] $\lambda$6584 emission lines enables an investigation of the $\mathrm{C/O}$, $\mathrm{N/O}$, and $\mathrm{C/N}$ abundance ratios using the temperature-sensitive method. The galaxies have stellar masses of ${\mathrm{log}(M_{\star}/\mathrm{M}_{\odot}) = 8.09^{+\, 0.24}_{-0.15}}$ and ${\mathrm{log}(M_{\star}/\mathrm{M}_{\odot}) = 8.02^{+\, 0.06}_{-0.08}}$ with metallicities of $Z \simeq 0.2 \, \rm{Z_{\odot}}$ and $Z \simeq 0.3 \, \rm{Z_{\odot}}$. These metallicities are somewhat higher than is typical for other $z\gtrsim 5$ galaxies with similar stellar mass and are comparable to $z \simeq 0$ analogues. Both galaxies display evidence for elevated N/O ratios with respect to the typical star-forming galaxies at $z\simeq0$, with ${\mathrm{log(N/O)} = -1.07^{+\,0.17}_{-0.13}}$ and ${\mathrm{log(N/O)} = -0.86^{+\,0.15}_{-0.11}}$ respectively. In contrast, we find low C abundances, with ${\mathrm{log(C/O)}=-0.82\pm0.22}$ and ${\mathrm{log(C/O)}=-1.02\pm0.22}$, consistent with the predicted yields of core-collapse supernovae. Following the trend observed in other high-redshift sources, we find that the $\mathrm{C/N}$ ratios are lower at fixed $\mathrm{O/H}$ compared to the majority of local galaxies. Via a comparison to detailed chemical evolution models, we find that a standard or bottom-heavy IMF can explain the observed abundance ratios where the N-enrichment comes from intermediate mass ($\simeq 4-7 \, \mathrm{M}_{\odot}$) stars. Our results demonstrate that robust measurements of CNO abundances with \emph{JWST} can reveal unique enrichment pathways in galaxies as a function of both metallicity and redshift.

Figures

Figures reproduced from arXiv: 2412.10557 by the authors.

Figure 1
Figure 1. Rest-frame UV and optical NIRSpec spectra of EXCELS-70864 at 𝑧 = 5.255. The black and grey line show the spectrum and error spectrum respectively. We highlight the detection of some UV and optical features such as C iii] 𝜆1906,1909, [O ii] 𝜆𝜆3726,29, [Ne iii] 𝜆3869, [O iii] 𝜆4363, [N ii] 𝜆6584, and [S ii] 𝜆𝜆6717,31, which are used to determine the physical conditions, chemical abundances and physical properties of E… view at source ↗
Figure 2
Figure 2. Rest-frame UV and optical NIRSpec spectra of EXCELS-121806 at 𝑧 = 5.255. For more details see Fig.1. for galaxies at 𝑧 > 6 and by Scarlata et al. (2024) for galaxies at 𝑧 ≃ 0. For example, McClymont et al. (2024) analyzed the cause of anomalous H𝛼/H𝛽 and H𝛾/H𝛽 ratios using 19 galaxies from JADES. With the aid of photoionisation models, these authors con￾clude that a density-bounded nebula is one of the possible expl… view at source ↗
Figure 3
Figure 3. The observed Balmer ratios of the EXCELS galaxies at 𝑧 ≃ 5. The red rectangles represent the theoretical Balmer ratios under the conditions of 𝑇𝑒 = 10 000 K − 20 000 K and 𝑛𝑒 = 300 cm−3 . Top panel: H𝛼/H𝛽 versus H𝛾/H𝛽. Both galaxies display H𝛼/H𝛽 ratios below the Case B value while the H𝛾/H𝛽 ratios are consistent with the Case B value or a small amount of nebular reddening. Bottom: H𝛼/H𝛽 versus H𝛿/H𝛽. Again the EXCE… view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: The [N ii] (left) and [S ii] (right) BPT diagrams for the EXCELS galaxies and a selection of literature samples. For EXCELS-70864, we have determined an upper limit for [S ii]/H𝛼. The solid line shows the theoretical maximum starburst separation of Kewley et al. (2001)…
Figure 5
Figure 5. Figure 5: Left: The SFR versus stellar mass relation for the EXCELS galaxies at 𝑧 ≃ 5 (red stars), along with an additional sample from the literature. Star-forming galaxies at 𝑧 ≃ 0 galaxies (circles) are taken from Berg et al. (2016, 2019a); Izotov et al. (2023); Ravindranath …
Figure 6
Figure 6. Figure 6: Left-hand panel: The N/O − O/H values for the EXCELS galaxies (red stars) compared with SFGs at different cosmic epochs. The circles represent galaxies at 𝑧 ≃ 0 (Berg et al. 2016, 2019a; Ravindranath et al. 2020; Senchyna et al. 2021; Berg et al. 2022; Izotov et al. 20…
Figure 7
Figure 7. Figure 7: The C/N − O/H relationship for the EXCELS galaxies at 𝑧 ≃ 5 compared to literature samples. The sample of local dwarf SFGs and LCEs are represented with circles (Berg et al. 2012; Berg et al. 2016; Izotov et al. 2023; Arellano-Córdova et al. in prep; Martinez et al. in…
Figure 8
Figure 8. Figure 8: Chemical evolution models illustrating the affect of different IMFs on the C/N abundance ratios. Top panel: A set of representative star￾formation histories assuming a shallow IMF (𝑥 = 1.1; black dashed line), a Kroupa (2001) IMF (𝑥 = 1.3; red solid line), and a steepe…

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Forward citations

Cited by 9 Pith papers

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Reference graph

Works this paper leans on

126 extracted references · 5 canonical work pages · cited by 9 Pith papers

  1. [1]

    G., Groves B

    Allen M. G., Groves B. A., Dopita M. A., Sutherland R. S., Kewley L. J., 2008, , 178, 20

    2008

  2. [2]

    O., P \'e rez-Montero E., V \' lchez J

    Amor \' i n R. O., P \'e rez-Montero E., V \' lchez J. M., 2010, , 715, L128

    2010

  3. [3]

    Z., Rodr \'i guez M., 2020, @doi [ ] 10.1093/mnras/staa1759 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.497..672A 497, 672

    Arellano-C \'o rdova K. Z., Rodr \'i guez M., 2020, @doi [ ] 10.1093/mnras/staa1759 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.497..672A 497, 672

    doi:10.1093/mnras/staa1759 2020

  4. [4]

    Z., et al., 2022, @doi [ ] 10.3847/2041-8213/ac9ab2 , https://ui.adsabs.harvard.edu/abs/2022ApJ...940L..23A 940, L23

    Arellano-C \'o rdova K. Z., et al., 2022, @doi [ ] 10.3847/2041-8213/ac9ab2 , https://ui.adsabs.harvard.edu/abs/2022ApJ...940L..23A 940, L23

    doi:10.3847/2041-8213/ac9ab2 2022

  5. [5]

    Z., et al., 2024, @doi [ ] 10.3847/1538-4357/ad34cf , https://ui.adsabs.harvard.edu/abs/2024ApJ...968...98A 968, 98

    Arellano-C \'o rdova K. Z., et al., 2024, @doi [ ] 10.3847/1538-4357/ad34cf , https://ui.adsabs.harvard.edu/abs/2024ApJ...968...98A 968, 98

    doi:10.3847/1538-4357/ad34cf 2024

  6. [6]

    M., Grevesse N., 2021, @doi [ ] 10.1051/0004-6361/202140445 , https://ui.adsabs.harvard.edu/abs/2021A&A...653A.141A 653, A141

    Asplund M., Amarsi A. M., Grevesse N., 2021, @doi [ ] 10.1051/0004-6361/202140445 , https://ui.adsabs.harvard.edu/abs/2021A&A...653A.141A 653, A141

    doi:10.1051/0004-6361/202140445 2021

  7. [7]

    Astropy Collaboration et al., 2018, @doi [aj] 10.3847/1538-3881/aabc4f , https://ui.adsabs.harvard.edu/abs/2018AJ....156..123A 156, 123

    doi:10.3847/1538-3881/aabc4f 2018

  8. [8]

    M., Lim P

    Astropy Collaboration Price-Whelan A. M., Lim P. L., et al., 2022, @doi [ ] 10.3847/1538-4357/ac7c74 , https://ui.adsabs.harvard.edu/abs/2022ApJ...935..167A 935, 167

    doi:10.3847/1538-4357/ac7c74 2022

Show all 126 references
  1. [9]

    A., Phillips M

    Baldwin J. A., Phillips M. M., Terlevich R., 1981, , 93, 5

    1981

  2. [10]

    Bekki K., Tsujimoto T., 2023, @doi [ ] 10.1093/mnrasl/slad108 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.526L..26B 526, L26

    2023 doi

  3. [11]

    A., Skillman E

    Berg D. A., Skillman E. D., Marble A., et al., 2012, , 754, 98

    2012

  4. [12]

    A., Skillman E

    Berg D. A., Skillman E. D., Henry R. B. C., Erb D. K., Carigi L., 2016, , 827, 126

    2016

  5. [13]

    A., Erb D

    Berg D. A., Erb D. K., Auger M. W., Pettini M., Brammer G. B., 2018, , 859, 164

    2018

  6. [14]

    A., Erb D

    Berg D. A., Erb D. K., Henry R. B. C., Skillman E. D., McQuinn K. B. W., 2019a, @doi [ ] 10.3847/1538-4357/ab020a , http://adsabs.harvard.edu/abs/2019ApJ...874...93B 874, 93

    doi

  7. [15]

    A., Chisholm J., Erb D

    Berg D. A., Chisholm J., Erb D. K., Pogge R., Henry A., et al., 2019b, @doi [ ] 10.3847/2041-8213/ab21dc , https://ui.adsabs.harvard.edu/abs/2019ApJ...878L...3B 878, L3

    doi

  8. [16]

    A., Chisholm J., Erb D

    Berg D. A., Chisholm J., Erb D. K., Skillman E. D., Pogge R. W., Olivier G. M., 2021, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2021arXiv210512765B p. arXiv:2105.12765

    2021 arXiv

  9. [17]

    A., et al., 2022, @doi [ ] 10.3847/1538-4365/ac6c03 , https://ui.adsabs.harvard.edu/abs/2022ApJS..261...31B 261, 31

    Berg D. A., et al., 2022, @doi [ ] 10.3847/1538-4365/ac6c03 , https://ui.adsabs.harvard.edu/abs/2022ApJS..261...31B 261, 31

    2022 doi

  10. [18]

    A., Burke P

    Berrington K. A., Burke P. G., Dufton P. L., Kingston A. E., 1985, @doi [Atomic Data and Nuclear Data Tables] 10.1016/0092-640X(85)90001-4 , https://ui.adsabs.harvard.edu/abs/1985ADNDT..33..195B 33, 195

    1985 doi

  11. [19]

    Bertin E., Arnouts S., 1996, @doi [ ] 10.1051/aas:1996164 , https://ui.adsabs.harvard.edu/abs/1996A&AS..117..393B 117, 393

    1996 doi

  12. [20]

    Bruzual G., Charlot S., 2003, @doi [ ] 10.1046/j.1365-8711.2003.06897.x , https://ui.adsabs.harvard.edu/abs/2003MNRAS.344.1000B 344, 1000

    2003

  13. [21]

    J., et al., 2023, @doi [arXiv e-prints] 10.48550/arXiv.2302.07256 , https://ui.adsabs.harvard.edu/abs/2023arXiv230207256B p

    Bunker A. J., et al., 2023, @doi [arXiv e-prints] 10.48550/arXiv.2302.07256 , https://ui.adsabs.harvard.edu/abs/2023arXiv230207256B p. arXiv:2302.07256

    2023 doi arXiv

  14. [22]

    J., Katz H., Rey M

    Cameron A. J., Katz H., Rey M. P., Saxena A., 2023, @doi [arXiv e-prints] 10.48550/arXiv.2302.10142 , https://ui.adsabs.harvard.edu/abs/2023arXiv230210142C p. arXiv:2302.10142

    2023 doi arXiv

  15. [23]

    A., Clayton G

    Cardelli J. A., Clayton G. C., Mathis J. S., 1989, , 345, 245

    1989

  16. [24]

    C., McLure R

    Carnall A. C., McLure R. J., Dunlop J. S., Dav \'e R., 2018, @doi [ ] 10.1093/mnras/sty2169 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.480.4379C 480, 4379

    2018 doi

  17. [25]

    C., Leja J., Johnson B

    Carnall A. C., Leja J., Johnson B. D., McLure R. J., Dunlop J. S., Conroy C., 2019, @doi [ ] 10.3847/1538-4357/ab04a2 , https://ui.adsabs.harvard.edu/abs/2019ApJ...873...44C 873, 44

    2019 doi

  18. [26]

    C., et al., 2024, @doi [ ] 10.1093/mnras/stae2092 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.534..325C 534, 325

    Carnall A. C., et al., 2024, @doi [ ] 10.1093/mnras/stae2092 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.534..325C 534, 325

    2024 doi

  19. [27]

    arXiv:2403.10238

    Castellano M., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2403.10238 , https://ui.adsabs.harvard.edu/abs/2024arXiv240310238C p. arXiv:2403.10238

    2024 doi arXiv

  20. [28]

    Charbonnel C., Schaerer D., Prantzos N., Ram \' rez-Galeano L., Fragos T., Kuruvanthodi A., Marques-Chaves R., Gieles M., 2023, @doi [ ] 10.1051/0004-6361/202346410 , https://ui.adsabs.harvard.edu/abs/2023A&A...673L...7C 673, L7

    2023 doi

  21. [29]

    A., Erb D

    Citro A., Berg D. A., Erb D. K., Auger M. W., Becker G. D., James B. L., Skillman E. D., 2024, @doi [ ] 10.3847/1538-4357/ad4600 , https://ui.adsabs.harvard.edu/abs/2024ApJ...969..148C 969, 148

    2024 doi

  22. [30]

    E., Sanders R

    Clarke L., Shapley A. E., Sanders R. L., Topping M. W., Brammer G. B., Bento T., Reddy N. A., Kehoe E., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2406.05178 , https://ui.adsabs.harvard.edu/abs/2024arXiv240605178C p. arXiv:2406.05178

    2024 doi arXiv

  23. [31]

    V., Pogge R

    Croxall K. V., Pogge R. W., Berg D. A., Skillman E. D., Moustakas J., 2016, , 830, 4

    2016

  24. [32]

    Cullen F., et al., 2019, @doi [ ] 10.1093/mnras/stz1402 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.487.2038C 487, 2038

    2019 doi

  25. [33]

    Cullen F., et al., 2021, @doi [ ] 10.1093/mnras/stab1340 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.505..903C 505, 903

    2021 doi

  26. [34]

    Curti M., Mannucci F., Cresci G., Maiolino R., 2020, @doi [ ] 10.1093/mnras/stz2910 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.491..944C 491, 944

    2020 doi

  27. [35]

    arXiv:2407.02575

    Curti M., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2407.02575 , https://ui.adsabs.harvard.edu/abs/2024arXiv240702575C p. arXiv:2407.02575

    2024 doi arXiv

  28. [36]

    D'Eugenio F., et al., 2024, @doi [ ] 10.1051/0004-6361/202348636 , https://ui.adsabs.harvard.edu/abs/2024A&A...689A.152D 689, A152

    2024 doi

  29. [37]

    M., Dufour R

    De Robertis M. M., Dufour R. J., Hunt R. W., 1987, , 81, 195

    1987

  30. [38]

    L., et al., 2013, @doi [ ] 10.1093/mnras/stt610 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.432.2512D 432, 2512

    Dors O. L., et al., 2013, @doi [ ] 10.1093/mnras/stt610 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.432.2512D 432, 2512

    2013 doi

  31. [39]

    T., Rodr \' guez M., Carigi L., 2005, @doi [ ] 10.1086/426889 , https://ui.adsabs.harvard.edu/abs/2005ApJ...618L..95E 618, L95

    Esteban C., Garc \' a-Rojas J., Peimbert M., Peimbert A., Ruiz M. T., Rodr \' guez M., Carigi L., 2005, @doi [ ] 10.1086/426889 , https://ui.adsabs.harvard.edu/abs/2005ApJ...618L..95E 618, L95

    2005 doi

  32. [40]

    Florido E., Zurita A., P \'e rez-Montero E., 2022, @doi [ ] 10.1093/mnras/stac919 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.513.2006F 513, 2006

    2022 doi

  33. [41]

    R., et al., 2022, @doi [ ] 10.3847/1538-4365/ac5331 , https://ui.adsabs.harvard.edu/abs/2022ApJS..260....1F 260, 1

    Flury S. R., et al., 2022, @doi [ ] 10.3847/1538-4365/ac5331 , https://ui.adsabs.harvard.edu/abs/2022ApJS..260....1F 260, 1

    2022 doi

  34. [42]

    R., Arellano-C \'o rdova K

    Flury S. R., Arellano-C \'o rdova K. Z., Moran E. C., Einsig A., 2024, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2024arXiv241206763F p. arXiv:2412.06763

    2024

  35. [43]

    R., 1990, , 363, 142

    Garnett D. R., 1990, , 363, 142

    1990

  36. [44]

    R., 1992, , 103, 1330

    Garnett D. R., 1992, , 103, 1330

    1992

  37. [45]

    Glass R., 1983, @doi [ ] 10.1007/BF00651295 , https://ui.adsabs.harvard.edu/abs/1983Ap&SS..92..307G 92, 307

    1983 doi

  38. [46]

    D., Clayton G

    Gordon K. D., Clayton G. C., Misselt K. A., Landolt A. U., Wolff M. J., 2003, @doi [ ] 10.1086/376774 , https://ui.adsabs.harvard.edu/abs/2003ApJ...594..279G 594, 279

    2003 doi

  39. [47]

    Hayden-Pawson C., et al., 2022, @doi [ ] 10.1093/mnras/stac584 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.512.2867H 512, 2867

    2022 doi

  40. [48]

    E., et al., 2023, @doi [ ] 10.1051/0004-6361/202347418 , https://ui.adsabs.harvard.edu/abs/2023A&A...679A..91H 679, A91

    Heintz K. E., et al., 2023, @doi [ ] 10.1051/0004-6361/202347418 , https://ui.adsabs.harvard.edu/abs/2023A&A...679A..91H 679, A91

    2023 doi

  41. [49]

    Henry R. B. C., Edmunds M. G., K\"oppen J., 2000, , 541, 660

    2000

  42. [50]

    Horne K., 1986, @doi [ ] 10.1086/131801 , https://ui.adsabs.harvard.edu/abs/1986PASP...98..609H 98, 609

    1986 doi

  43. [51]

    Y.-Y., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2409.04625 , https://ui.adsabs.harvard.edu/abs/2024arXiv240904625H p

    Hsiao T. Y.-Y., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2409.04625 , https://ui.adsabs.harvard.edu/abs/2024arXiv240904625H p. arXiv:2409.04625

    2024 doi

  44. [52]

    arXiv:2401.12402

    Hu W., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2401.12402 , https://ui.adsabs.harvard.edu/abs/2024arXiv240112402H p. arXiv:2401.12402

    2024 doi arXiv

  45. [53]

    D., 2007, @doi [Computing in Science Engineering] 10.1109/MCSE.2007.55 , 9, 90

    Hunter J. D., 2007, @doi [Computing in Science Engineering] 10.1109/MCSE.2007.55 , 9, 90

    2007 doi

  46. [54]

    Isobe Y., Ouchi M., Nakajima K., Harikane Y., Ono Y., Xu Y., Zhang Y., Umeda H., 2023a, @doi [ ] 10.3847/1538-4357/acf376 , https://ui.adsabs.harvard.edu/abs/2023ApJ...956..139I 956, 139

    doi

  47. [55]

    Isobe Y., et al., 2023b, @doi [ ] 10.3847/1538-4357/ad09be , https://ui.adsabs.harvard.edu/abs/2023ApJ...959..100I 959, 100

    doi

  48. [56]

    I., Stasi \'n ska G., Meynet G., Guseva N

    Izotov Y. I., Stasi \'n ska G., Meynet G., Guseva N. G., Thuan T. X., 2006, , 448, 955

    2006

  49. [57]

    I., Schaerer D., Worseck G., Berg D., Chisholm J., Ravindranath S., Thuan T

    Izotov Y. I., Schaerer D., Worseck G., Berg D., Chisholm J., Ravindranath S., Thuan T. X., 2023, @doi [ ] 10.1093/mnras/stad1036 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.522.1228I 522, 1228

    2023 doi

  50. [58]

    L., et al., 2022, @doi [ ] 10.3847/1538-4365/ac8008 , https://ui.adsabs.harvard.edu/abs/2022ApJS..262...37J 262, 37

    James B. L., et al., 2022, @doi [ ] 10.3847/1538-4365/ac8008 , https://ui.adsabs.harvard.edu/abs/2022ApJS..262...37J 262, 37

    2022 doi

  51. [59]

    Ji X., et al., 2024, @doi [ ] 10.1093/mnras/stae2375 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.535..881J 535, 881

    2024 doi

  52. [60]

    Jones T., et al., 2023, @doi [ ] 10.3847/2041-8213/acd938 , https://ui.adsabs.harvard.edu/abs/2023ApJ...951L..17J 951, L17

    2023 doi

  53. [61]

    M., Tremonti C., et al., 2003, @doi [ ] 10.1111/j.1365-2966.2003.07154.x , 346, 1055

    Kauffmann G., Heckman T. M., Tremonti C., et al., 2003, @doi [ ] 10.1111/j.1365-2966.2003.07154.x , 346, 1055

    2003

  54. [62]

    Kennicutt Jr. R. C., Bresolin F., Garnett D. R., 2003, , 591, 801

    2003

  55. [63]

    J., Dopita M

    Kewley L. J., Dopita M. A., Sutherland R. S., Heisler C. A., Trevena J., 2001, , 556, 121

    2001

  56. [64]

    J., Jansen R

    Kewley L. J., Jansen R. A., Geller M. J., 2005, , 117, 227

    2005

  57. [65]

    pp 87 -- 90

    Kluyver T., et al., 2016, in Loizides F., Schmidt B., eds, Positioning and Power in Academic Publishing: Players, Agents and Agendas. pp 87 -- 90

    2016

  58. [66]

    Kobayashi C., Ferrara A., 2024, @doi [ ] 10.3847/2041-8213/ad1de1 , https://ui.adsabs.harvard.edu/abs/2024ApJ...962L...6K 962, L6

    2024 doi

  59. [67]

    I., Umeda H., 2011, , 414, 3231

    Kobayashi C., Karakas A. I., Umeda H., 2011, , 414, 3231

    2011

  60. [68]

    I., Lugaro M., 2020, @doi [ ] 10.3847/1538-4357/abae65 , https://ui.adsabs.harvard.edu/abs/2020ApJ...900..179K 900, 179

    Kobayashi C., Karakas A. I., Lugaro M., 2020, @doi [ ] 10.3847/1538-4357/abae65 , https://ui.adsabs.harvard.edu/abs/2020ApJ...900..179K 900, 179

    2020 doi

  61. [69]

    Kroupa P., 2001, @doi [ ] 10.1046/j.1365-8711.2001.04022.x , https://ui.adsabs.harvard.edu/abs/2001MNRAS.322..231K 322, 231

    2001

  62. [70]

    arXiv:2303.01536

    Llerena M., et al., 2023, @doi [arXiv e-prints] 10.48550/arXiv.2303.01536 , https://ui.adsabs.harvard.edu/abs/2023arXiv230301536L p. arXiv:2303.01536

    2023 doi arXiv

  63. [71]

    A., 2015, , 573, A42

    Luridiana V., Morisset C., Shaw R. A., 2015, , 573, A42

    2015

  64. [72]

    Maiolino R., et al., 2024, @doi [ ] 10.1038/s41586-024-07052-5 , https://ui.adsabs.harvard.edu/abs/2024Natur.627...59M 627, 59

    2024 doi

  65. [73]

    arXiv:2307.04234

    Marques-Chaves R., et al., 2023, @doi [arXiv e-prints] 10.48550/arXiv.2307.04234 , https://ui.adsabs.harvard.edu/abs/2023arXiv230704234M p. arXiv:2307.04234

    2023 doi arXiv

  66. [74]

    arXiv:2405.15859

    McClymont W., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2405.15859 , https://ui.adsabs.harvard.edu/abs/2024arXiv240515859M p. arXiv:2405.15859

    2024 doi

  67. [75]

    arXiv:2209.09047

    Mingozzi M., et al., 2022, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2022arXiv220909047M p. arXiv:2209.09047

    2022 arXiv

  68. [76]

    Mingozzi M., et al., 2024, @doi [ ] 10.3847/1538-4357/ad1033 , https://ui.adsabs.harvard.edu/abs/2024ApJ...962...95M 962, 95

    2024 doi

  69. [77]

    Morishita T., et al., 2024, @doi [ ] 10.3847/1538-4357/ad5290 , https://ui.adsabs.harvard.edu/abs/2024ApJ...971...43M 971, 43

    2024 doi

  70. [78]

    Moustakas J., Buhler J., Scholte D., Dey B., Khederlarian A., 2023, FastSpecFit: Fast spectral synthesis and emission-line fitting of DESI spectra , Astrophysics Source Code Library, record ascl:2308.005

    2023

  71. [79]

    Nakajima K., Ouchi M., Isobe Y., Harikane Y., Zhang Y., Ono Y., Umeda H., Oguri M., 2023, @doi [ ] 10.3847/1538-4365/acd556 , https://ui.adsabs.harvard.edu/abs/2023ApJS..269...33N 269, 33

    2023 doi

  72. [80]

    C., Sutherland R

    Nicholls D. C., Sutherland R. S., Dopita M. A., Kewley L. J., Groves B. A., 2017, , 466, 4403

    2017

  73. [81]

    J., 1978, , https://ui.adsabs.harvard.edu/abs/1978A&A....64..139N 64, 139

    Nussbaumer H., Storey P. J., 1978, , https://ui.adsabs.harvard.edu/abs/1978A&A....64..139N 64, 139

    1978

  74. [82]

    E., 1989, Astrophysics of gaseous nebulae and active galactic nuclei

    Osterbrock D. E., 1989, Astrophysics of gaseous nebulae and active galactic nuclei

    1989

  75. [83]

    E., Ferland G

    Osterbrock D. E., Ferland G. J., 2006, Astrophysics of gaseous nebulae and active galactic nuclei

    2006

  76. [84]

    Virtanen R

    P. Virtanen R. Gommers T. O., 2020, @doi [Nature Methods] https://doi.org/10.1038/s41592-019-0686-2 , 17, 261

    2020 doi

  77. [85]

    F., Tsang B

    Pascale M., Dai L., McKee C. F., Tsang B. T. H., 2023, @doi [ ] 10.3847/1538-4357/acf75c , https://ui.adsabs.harvard.edu/abs/2023ApJ...957...77P 957, 77

    2023 doi

  78. [86]

    A., Leitherer C., de Mink S., Wofford A., Kewley L., 2017, , 847, 107

    Pe \ n a-Guerrero M. A., Leitherer C., de Mink S., Wofford A., Kewley L., 2017, , 847, 107

    2017

  79. [87]

    Peimbert M., Costero R., 1969, Boletin de los Observatorios Tonantzintla y Tacubaya, 5, 3

    1969

  80. [88]

    Peimbert M., Peimbert A., Delgado-Inglada G., 2017, @doi [ ] 10.1088/1538-3873/aa72c3 , https://ui.adsabs.harvard.edu/abs/2017PASP..129h2001P 129, 082001

    2017 doi

  81. [89]

    P \'e rez-Montero E., Contini T., 2009, , 398, 949

    2009

  82. [90]

    F., Contini T., D \' az \'A

    P \'e rez-Montero E., H \"a gele G. F., Contini T., D \' az \'A . I., 2007, @doi [ ] 10.1111/j.1365-2966.2007.12213.x , https://ui.adsabs.harvard.edu/abs/2007MNRAS.381..125P 381, 125

    2007

  83. [91]

    C., Tumlinson J., 2020, @doi [ ] 10.3847/1538-4357/ab91a5 , https://ui.adsabs.harvard.edu/abs/2020ApJ...896..170R 896, 170

    Ravindranath S., Monroe T., Jaskot A., Ferguson H. C., Tumlinson J., 2020, @doi [ ] 10.3847/1538-4357/ab91a5 , https://ui.adsabs.harvard.edu/abs/2020ApJ...896..170R 896, 170

    2020 doi

  84. [92]

    A., et al., 2018, @doi [ ] 10.3847/1538-4357/aaed1e , https://ui.adsabs.harvard.edu/abs/2018ApJ...869...92R 869, 92

    Reddy N. A., et al., 2018, @doi [ ] 10.3847/1538-4357/aaed1e , https://ui.adsabs.harvard.edu/abs/2018ApJ...869...92R 869, 92

    2018 doi

  85. [93]

    E., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2404.08884 , https://ui.adsabs.harvard.edu/abs/2024arXiv240408884R p

    Rivera-Thorsen T. E., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2404.08884 , https://ui.adsabs.harvard.edu/abs/2024arXiv240408884R p. arXiv:2404.08884

    2024 doi arXiv

  86. [94]

    Rogers N. S. J., Skillman E. D., Pogge R. W., Berg D. A., Moustakas J., Croxall K. V., Sun J., 2021, @doi [ ] 10.3847/1538-4357/abf8b9 , https://ui.adsabs.harvard.edu/abs/2021ApJ...915...21R 915, 21

    2021 doi

  87. [95]

    Rogers N. S. J., Strom A. L., Rudie G. C., Trainor R. F., Raptis M., von Raesfeld C., 2024, @doi [ ] 10.3847/2041-8213/ad2f37 , https://ui.adsabs.harvard.edu/abs/2024ApJ...964L..12R 964, L12

    2024 doi

  88. [96]

    C., 2018, @doi [ ] 10.3847/1538-4357/aabf3c , https://ui.adsabs.harvard.edu/abs/2018ApJ...859...11S 859, 11

    Salim S., Boquien M., Lee J. C., 2018, @doi [ ] 10.3847/1538-4357/aabf3c , https://ui.adsabs.harvard.edu/abs/2018ApJ...859...11S 859, 11

    2018 doi

  89. [97]

    L., Jones T., others 2022,

    Sanders R. L., Jones T., others 2022,

    2022

  90. [98]

    L., et al., 2023a, @doi [ ] 10.3847/1538-4357/aca9cc , https://ui.adsabs.harvard.edu/abs/2023ApJ...943...75S 943, 75

    Sanders R. L., et al., 2023a, @doi [ ] 10.3847/1538-4357/aca9cc , https://ui.adsabs.harvard.edu/abs/2023ApJ...943...75S 943, 75

    doi

  91. [99]

    L., Shapley A

    Sanders R. L., Shapley A. E., Topping M. W., Reddy N. A., Brammer G. B., 2023b, @doi [ ] 10.3847/1538-4357/acedad , https://ui.adsabs.harvard.edu/abs/2023ApJ...955...54S 955, 54

    doi

  92. [100]

    L., Shapley A

    Sanders R. L., Shapley A. E., Topping M. W., Reddy N. A., Brammer G. B., 2024, @doi [ ] 10.3847/1538-4357/ad15fc , https://ui.adsabs.harvard.edu/abs/2024ApJ...962...24S 962, 24

    2024 doi

  93. [101]

    arXiv:2404.09015

    Scarlata C., Hayes M., Panagia N., Mehta V., Haardt F., Bagley M., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2404.09015 , https://ui.adsabs.harvard.edu/abs/2024arXiv240409015S p. arXiv:2404.09015

    2024 doi arXiv

  94. [102]

    arXiv:2406.08408

    Schaerer D., Marques-Chaves R., Xiao M., Korber D., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2406.08408 , https://ui.adsabs.harvard.edu/abs/2024arXiv240608408S p. arXiv:2406.08408

    2024 doi arXiv

  95. [103]

    arXiv:2502.10499

    Scholte D., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2502.10499 , https://ui.adsabs.harvard.edu/abs/2025arXiv250210499S p. arXiv:2502.10499

    2025 doi arXiv

  96. [104]

    arXiv:2111.11508

    Senchyna P., et al., 2021, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2021arXiv211111508S p. arXiv:2111.11508

    2021 arXiv

  97. [105]

    P., Rudie G

    Senchyna P., Plat A., Stark D. P., Rudie G. C., 2023, @doi [arXiv e-prints] 10.48550/arXiv.2303.04179 , https://ui.adsabs.harvard.edu/abs/2023arXiv230304179S p. arXiv:2303.04179

    2023 doi arXiv

  98. [106]

    E., Reddy N

    Shapley A. E., Reddy N. A., Kriek M., et al., 2015, , 801, 88

    2015

  99. [107]

    E., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2407.00157 , https://ui.adsabs.harvard.edu/abs/2024arXiv240700157S p

    Shapley A. E., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2407.00157 , https://ui.adsabs.harvard.edu/abs/2024arXiv240700157S p. arXiv:2407.00157

    2024 doi arXiv

  100. [108]

    D., Berg D

    Skillman E. D., Berg D. A., Pogge R. W., Moustakas J., Rogers N. S. J., Croxall K. V., 2020, @doi [ ] 10.3847/1538-4357/ab86ae , https://ui.adsabs.harvard.edu/abs/2020ApJ...894..138S 894, 138

    2020 doi

  101. [109]

    M., et al., 2024, @doi [ ] 10.1093/mnras/stae1705 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.532.3102S 532, 3102

    Stanton T. M., et al., 2024, @doi [ ] 10.1093/mnras/stae1705 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.532.3102S 532, 3102

    2024 doi

  102. [110]

    M., et al., 2025, @doi [ ] 10.1093/mnras/staf106 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.537.1735S 537, 1735

    Stanton T. M., et al., 2025, @doi [ ] 10.1093/mnras/staf106 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.537.1735S 537, 1735

    2025 doi

  103. [111]

    Stasi \'n ska G., 1982, , 48, 299

    1982

  104. [112]

    C., Rudie G

    Steidel C. C., Rudie G. C., Strom A. L., et al., 2014, , 795, 165

    2014

  105. [113]

    C., Strom A

    Steidel C. C., Strom A. L., Pettini M., Rudie G. C., Reddy N. A., Trainor R. F., 2016, , 826, 159

    2016

  106. [114]

    W., Shapley A

    Topping M. W., Shapley A. E., Reddy N. A., Sanders R. L., Coil A. L., et al., 2020, @doi [ ] 10.1093/mnras/staa1410 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.495.4430T 495, 4430

    2020 doi

  107. [115]

    W., et al., 2024a, @doi [arXiv e-prints] 10.48550/arXiv.2407.19009 , https://ui.adsabs.harvard.edu/abs/2024arXiv240719009T p

    Topping M. W., et al., 2024a, @doi [arXiv e-prints] 10.48550/arXiv.2407.19009 , https://ui.adsabs.harvard.edu/abs/2024arXiv240719009T p. arXiv:2407.19009

    doi arXiv

  108. [116]

    W., et al., 2024b, @doi [ ] 10.1093/mnras/stae682 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.529.3301T 529, 3301

    Topping M. W., et al., 2024b, @doi [ ] 10.1093/mnras/stae682 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.529.3301T 529, 3301

    doi

  109. [117]

    Vincenzo F., Belfiore F., Maiolino R., Matteucci F., Ventura P., 2016, @doi [ ] 10.1093/mnras/stw532 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.458.3466V 458, 3466

    2016 doi

  110. [118]

    S., 2023, @doi [ ] 10.1051/0004-6361/202347827 , https://ui.adsabs.harvard.edu/abs/2023A&A...679L...9V 679, L9

    Vink J. S., 2023, @doi [ ] 10.1051/0004-6361/202347827 , https://ui.adsabs.harvard.edu/abs/2023A&A...679L...9V 679, L9

    2023 doi

  111. [119]

    Watanabe K., et al., 2024, @doi [ ] 10.3847/1538-4357/ad13ff , https://ui.adsabs.harvard.edu/abs/2024ApJ...962...50W 962, 50

    2024 doi

  112. [120]

    arXiv:2405.06631

    Welch B., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2405.06631 , https://ui.adsabs.harvard.edu/abs/2024arXiv240506631W p. arXiv:2405.06631

    2024 doi arXiv

  113. [121]

    L., Fuhr J

    Wiese W. L., Fuhr J. R., Deters T. M., 1996, Atomic transition probabilities of carbon, nitrogen, and oxygen : a critical data compilation

    1996

  114. [122]

    Yan Z., Jerabkova T., Kroupa P., 2017, @doi [ ] 10.1051/0004-6361/201730987 , https://ui.adsabs.harvard.edu/abs/2017A&A...607A.126Y 607, A126

    2017 doi

  115. [123]

    arXiv:2403.20118

    Yanagisawa H., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2403.20118 , https://ui.adsabs.harvard.edu/abs/2024arXiv240320118Y p. arXiv:2403.20118

    2024 doi arXiv

  116. [124]

    van Dokkum P., Conroy C., 2024, @doi [ ] 10.3847/2041-8213/ad77b8 , https://ui.adsabs.harvard.edu/abs/2024ApJ...973L..32V 973, L32

    2024 doi

  117. [125]

    C., Varoquaux G., 2011, @doi [Computing in Science Engineering] 10.1109/MCSE.2011.37 , 13, 22

    van der Walt S., Colbert S. C., Varoquaux G., 2011, @doi [Computing in Science Engineering] 10.1109/MCSE.2011.37 , 13, 22

    2011 doi

  118. [126]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.stat...

Pith tools

Reviewed August 11, 2026 · model on record in the stance chip above.