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DESI's deep spectra make direct chemical abundances routine for ~50,000 star-forming galaxies, revealing two record-low metallicity systems.

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2026-08-03 12:30 UTC pith:WN2GDWTT

load-bearing objection The catalogue is the real advance; the second record galaxy is on shakier ground than the first. the 3 major comments →

arxiv 2601.02463 v2 pith:WN2GDWTT submitted 2026-01-05 astro-ph.GA

Electron temperature relations and the direct N, O, Ne, S and Ar abundances of 49959 star-forming galaxies in DESI Data Release 2

D. Scholte , F. Cullen , J. Moustakas , H. Zou , A. Saintonge , K. Z. Arellano-Cordova , T. M. Stanton , B. Andrews
show 37 more authors
J. Sui J. Aguilar S. Ahlen D. Bianchi D. Brooks F. J. Castander T. Cheng T. Claybaugh A. de la Macorra B. Dey P. Doel K. Douglass S. Ferraro J. E. Forero-Romero E. Gazta\~naga S. Gontcho A Gontcho G. Gutierrez R. Joyce A. Kremin O. Lahav M. Landriau L. Le Guillou P. Martini A. Meisner R. Miquel W. J. Percival C. Poppett F. Prada I. P\'erez-R\`afols G. Rossi E. Sanchez D. Schlegel Z. Shao J. Silber D. Sprayberry G. Tarl\'e B. A. Weaver
This is my paper
classification astro-ph.GA
keywords direct electron temperaturesauroral emission lineschemical abundancesstar-forming galaxiesextremely metal-poor galaxiesabundance ratiosDESI surveyionisation correction factors
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This paper claims to have built the largest catalogue of direct-method galaxy abundances to date: 49,959 star-forming galaxies from DESI Data Release 2 with electron-temperature measurements, and direct oxygen abundances for 49,507 of them. The sample is roughly two orders of magnitude larger than previous direct-method samples, which is what lets the authors isolate rare objects and weak trends. Within it they find two galaxies with oxygen abundances of about 1.2% and 1.3% solar—the lowest confirmed direct measurements yet—along with 3,114 extremely metal-poor galaxies below 10% solar. The paper also maps how N/O, Ne/O, S/O, and Ar/O vary with metallicity, finding a flat-then-rising Ne/O trend and a tight S/O–Ar/O correlation. A sympathetic reader would see this as turning the gold-standard direct method from a small-sample technique into a survey-scale statistical tool.

Core claim

We present the largest direct-method abundance catalogue of star-forming galaxies yet assembled: 49,959 galaxies from DESI Data Release 2 with electron-temperature measurements and direct oxygen abundances for 49,507. Detecting faint auroral lines and forward-modeling the ionized gas lets us measure temperatures in the high, intermediate, and low ionisation zones; our relation Te(S++) ≈ Te(O++) is close to one-to-one, and Te(O+) = 0.648×Te(O++) + 3,270 K. The sample contains the two most metal-poor confirmed galaxies in the nearby Universe — DESI J211.9086+28.2461 at 12+log(O/H)=6.77 and DESI J169.0571+14.1514 at 6.81 — plus 3,114 galaxies below 10% solar. Abundance ratios follow a constant

What carries the argument

The direct (auroral-line) method: electron temperatures are derived from faint forbidden lines ([OIII]4363, [SIII]6312, [NII]5755, [OII]7320/7330, [SII]4068). Where a temperature is missing in a given ionisation zone, literature temperature relations (T_low=0.7×T_high+3000 K; T_mid=1.265×T_high−2320 K) fill the gap; total N, Ne, S, Ar abundances use standard ionisation correction factors (Izotov et al. 2006). The sample size — roughly two orders of magnitude more auroral-line galaxies than any previous study — is itself the central tool: it makes rare populations (record-low metallicity, nitrogen-rich outliers) and subtle ratio trends statistically visible.

Load-bearing premise

The abundance scale for galaxies lacking a direct temperature in a given ionisation zone rests on the assumed electron-temperature relations and on the ionisation correction factors used to convert measured ions to total N, Ne, S, and Ar abundances; if those priors are wrong, the abundances and the Ne/O and S/O–Ar/O trends shift systematically.

What would settle it

Recompute the sample abundances with alternative ionisation correction factors (e.g., those of Pérez-Montero, Dors, or Amayo) and check whether the Ne/O rise at 12+log(O/H)>8.1 and the record-low metallicities survive; or obtain high-S/N spectra of DESI J211.9086+28.2461 and DESI J169.0571+14.1514 to verify the auroral-line detections and the [OII] non-detection.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Direct-method abundance measurements cease to be the bottleneck: the catalogue provides ~50,000 anchor points for calibrating strong-line metallicity diagnostics.
  • The two record-low galaxies (12+log(O/H)=6.77 and 6.81) become the new benchmark targets for studying nucleosynthesis and feedback in nearly pristine gas.
  • The N/O plateau and break (at 12+log(O/H)=8.142) sharpen constraints on nitrogen production timescales and gas recycling.
  • The S/O–Ar/O correlation supports Type Ia supernovae as a common secondary enrichment channel for both elements.
  • The 3,114 extremely metal-poor galaxies provide a local analogue population for interpreting high-redshift metallicity measurements.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the catalogue is correct, the community can re-derive strong-line calibrations (e.g., R23, O3N2) from a sample spanning 7.4<12+log(O/H)<8.85, substantially reducing the systematic floor of extragalactic metallicity measurements.
  • The Ne/O upturn is a plausible gas-phase tracer of oxygen depletion onto dust: a testable extension is to check whether the upturn strength correlates with independent dust-to-metal ratio estimates for the same galaxies.
  • The 139 high-N/O low-metallicity outliers suggest nitrogen-rich galaxies are more common locally than previously assumed, weakening the case that such abundance patterns uniquely signal exotic early-Universe conditions; comparing their stellar ages and masses to the general sample would test the gas-dilution picture.
  • High-S/N follow-up of the two record-low galaxies is the direct external check: a non-detection of their weak [OII] lines, or a different Te estimate, could shift them above the previous records.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. Scholte et al. present an emission-line analysis of DESI DR2 star-forming galaxies, using PyNeb forward modeling to derive electron temperatures, densities, and N, O, Ne, S, Ar abundances for 49,959 galaxies, of which ~49,766 have direct 12+log(O/H) measurements. They fit electron-temperature relations, compare with CLASSY and Zou et al. (2024), report 3,114 EMPGs, two record-low oxygen abundances (12+log(O/H)=6.77 and 6.81), 139 high-N/O outliers, a Ne/O upturn above 12+log(O/H)~8.1, and a S/O–Ar/O correlation. The catalogue is the main deliverable.

Significance. The strengths are substantial: selection thresholds, S/N cuts, residual-based line rejection, and Monte Carlo uncertainties are documented; the comparison with CLASSY and Zou et al. (2024) provides an external sanity check; the data model in Appendix A prepares for public release. If the catalogue is made public as described, it will be a new reference sample for Te-based abundance studies at z<0.96. The headline record-galaxy claim and the Ne/O upturn, however, need the additional quantitative support identified below.

major comments (3)
  1. [§4.3.1] The claim of 'two galaxies with metallicities lower than any previous confirmed direct measurements' rests on DESI J169.0571+14.1514, whose total O/H is derived from O++ alone because [OII] λλ3726,3729 is not detected. The manuscript says the non-detection 'suggests a negligible fraction' of O+, but no upper limit is quantified. With 12+log(O++/H)=6.81±0.04, an O+/O++ ratio of ~0.23 gives 12+log(O/H)=6.90, equal to the previous record HSC J1631+4426; such O+ fractions are common in low-metallicity galaxies. Please provide a quantitative upper limit on the [OII] doublet (or on O+/H+) from the spectrum or the fitted line model and propagate it into the total O/H, or restrict the record claim to DESI J211.9086+28.2461.
  2. [§4.3.3, Eq. (7)] The Ne/O upturn is presented as a result, but the paper itself states it 'could be due to inaccurate ICFs' — specifically the Izotov et al. (2006) ICFs adopted in §3.2, which also set the Ne/H and O/H values that define the trend. As a self-consistency check, please rederive the Ne/O relation with at least one alternative ICF set (e.g., Pérez-Montero et al. 2007; Dors et al. 2013; Amayo et al. 2021, already shown in Fig. 8) and report the resulting change in the break position and slope. Without this, the dust-depletion interpretation is not uniquely supported.
  3. [§3.2] Galaxies lacking a direct temperature in a given ionisation zone inherit the adopted literature T_e relations (Campbell et al. 1986 / Garnett 1992; Croxall et al. 2016), and N, Ne, S, Ar totals inherit the Izotov et al. (2006) ICFs. This is a reasonable and explicitly stated choice, but the paper does not quantify how much the final abundances would shift if the newly fitted temperature relations (Eqs. 2–4) were used instead. Since the catalogue is intended as a reference sample, a short systematic test on a representative subset—e.g., recomputing O/H and Ne/H with the new relations—would materially strengthen the usability of the catalogue.
minor comments (4)
  1. [Abstract / §4.3.2] The abstract states 24 high-N/O outliers, while the abstract in the main text and §4.3.2 state 139; also the front abstract gives 49,507 direct oxygen abundances while the main-text abstract and Table 4 give 49,766. Please reconcile these numbers.
  2. [Abstract] The phrase 'abundance ratios of as a function of metallicity' is missing a word; the sentence should read 'abundance ratios as a function of metallicity.' Several other places have missing 'are' (e.g., §4.3.1, '99% of our measurements between...').
  3. [§3.2 / Table 3] It would be helpful to state explicitly how many galaxies use each fiducial T_e relation (direct vs inferred temperature) in the final catalogue, so users can separate directly constrained from relation-inferred abundances.
  4. [§4.3.1] The detailed analysis of the two lowest-metallicity galaxies is deferred to Moustakas et al. (in prep.). For a paper making a record-breaking claim, the present manuscript should be as self-contained as possible; the quantitative upper limit requested above would address this.

Circularity Check

0 steps flagged

No significant circularity: Te measurements and abundances are derived from independent auroral-line detections; literature Te relations and ICFs are openly declared fiducial choices, not predictions.

full rationale

The central catalogue is built from direct emission-line measurements. Electron temperatures are inferred from auroral-to-strong-line ratios (Table 3) for ions where both lines are detected at S/N>3, and the posteriors are propagated into ionic abundances with PyNeb. For ionisation zones lacking a direct temperature, the paper explicitly adopts published relations (Campbell et al. 1986/Garnett 1992: T_low=0.7*T_high+3000K; Croxall et al. 2016) and Izotov et al. (2006) ICFs (Section 3.2), stating that this choice was made so results 'can be readily compared' with the literature. This is a transparent modelling assumption, not a result derived from its own output. The Te-Te relations in Section 4.1 (Eqs. 2-4) are fitted only to galaxies with direct measurements of both temperatures, so they are not fitting the fiducial relation back to itself. External comparisons (CLASSY, Zou et al. 2024, previous Te relations) provide independent checks. The record-low galaxy J169.0571+14.1514 relies on a non-detection of [OII] to justify a negligible O+ fraction; that is an observational weakness (no quantified upper limit) but not a circular reduction. The paper itself flags the Ne/O upturn 'could be due to inaccurate ICFs' (Section 4.3.3), an acknowledged systematic uncertainty rather than a circular step. Self-citations to in-preparation papers are for follow-up analysis and are not load-bearing. No equation reduces to its own input.

Axiom & Free-Parameter Ledger

6 free parameters · 8 axioms · 0 invented entities

The analysis rests on three kinds of upstream inputs: (i) literature electron-temperature relations and ICFs that map measured ionic lines to total abundances; (ii) atomic data and recombination/attenuation assumptions; (iii) sample-selection choices that bias the sample toward strongly star-forming galaxies. The fitted relations in §4 (N/O, Ne/O, S/O, Ar/O, Te–Te) are outputs of the analysis, but several are restated as findings while being fits, and the Ne/O interpretation leans on the very ICFs used to build the abundances.

free parameters (6)
  • N/O broken-linear relation parameters (c_plateau, c_break, c_slope) = -1.391±0.003, 8.142±0.014 dex, 1.02±0.06
    Fit by ODR to the sample (Eq. 6); characterizes the N/O–O/H relation and defines the high-N/O outlier selection boundary (12+log(O/H)<8.0).
  • Ne/O broken-linear relation parameters (c_plateau, c_break, c_slope) = -0.7499±0.0006, 8.105±0.004 dex, 0.250±0.004
    Fit to the sample in §4.3.3; the upturn at c_break=8.105 is a headline claim and depends on both the fit and the ICF choice.
  • Ne/O linear fit coefficients = slope 0.0970±0.0021, intercept -1.512±0.017
    Alternative description of the Ne/O–O/H relation (Eq. 7).
  • S/O and Ar/O linear fit coefficients = Eq. 8: 0.13±0.05, -2.74±0.04; Eq. 9: -0.112±0.004, -1.55±0.04
    Fit relations used to describe S/O and Ar/O versus O/H in §4.3.4.
  • Measured electron temperature relation coefficients (Eqs. 2–5) = e.g., Te(S++)=1.062×Te(O++)−0.06×10^4 K
    ODR fits used to propagate temperatures when a zone is not directly measured (e.g., Fig. 9 conversions).
  • Dust model parameters q_PAH, U_min, gamma = 1%, 1, 0.01
    Adopted from Draine et al. (2007) for dust emission in the SED fits (§2); chosen rather than fitted to the sample.
axioms (8)
  • domain assumption Fiducial Te relations: T_low=0.7×T_high+3000 K (Campbell 1986; Garnett 1992), T_mid=1.265×T_high−2320 K (Croxall 2016)
    Used in §3.2 to assign electron temperatures to ionization zones not directly constrained; the abundance scale inherits these relations.
  • domain assumption ICFs of Izotov et al. (2006), eqs. 18, 19, 20, 22, 23, convert measured ionic abundances to total N, Ne, S, Ar
    Used in §3.2; the paper acknowledges (§4.3.3) that the Ne/O upturn may be produced by the ICF choice.
  • domain assumption Three-zone ionization structure: high zone (O++, Ne++, Ar3+), intermediate (S++, Ar++), low (N+, O+, S+)
    Assumed in §3.2 following Mingozzi et al. 2022 and Berg et al. 2022.
  • domain assumption The contribution of O3+ (and higher O ions) to O/H is negligible
    §3.2: total O/H from O+ and O++ only, citing Berg et al. 2021 and Cullen et al. 2025.
  • standard math Case B recombination (Baker & Menzel 1938) and Cardelli et al. (1989) attenuation law with R_V=3.1
    Used in §3.1 to convert Balmer ratios to dust attenuation A_V.
  • standard math Atomic data (transition probabilities and collision strengths) as listed in Table 2
    PyNeb line-ratio modeling depends on these; e.g., Storey et al. 2014, Tayal & Zatsarinny 2010.
  • standard math Solar abundance scale of Asplund et al. (2021)
    Reference scale for 12+log(O/H) values and solar-metallicity fractions quoted in the paper.
  • domain assumption EW(Hβ)>20 Å and auroral-line S/N>5 cuts select star-forming galaxies dominated by HII regions rather than DIG
    §2; the paper notes the resulting sample is biased toward strongly star-forming galaxies (§4.3.1), weakening representativeness.

pith-pipeline@v1.3.0-alltime-deepseek · 32657 in / 18029 out tokens · 151777 ms · 2026-08-03T12:30:32.769598+00:00 · methodology

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read the original abstract

We present the largest direct-method abundance catalogue of galaxies to date, containing measurements of 49959 star-forming galaxies at z < 0.96 from DESI Data Release 2. By directly measuring electron temperatures across multiple ionisation zones, we provide constraints on a number of electron temperature relations. Using the temperature measurements, we derive reliable abundances for N, O, Ne, S and Ar and measure the evolution of abundances and abundance ratios of as a function of metallicity and other galaxy properties. Our measurements include direct oxygen abundances for 49507 galaxies, leading to the discovery of the two most metal-poor galaxies in the nearby Universe, with oxygen abundances of 12+log(O/H) = $\rm 12+\log(O/H) = 6.77_{-0.03}^{+0.03}~\rm dex $ (1.2\% $\rm Z_{\odot}$) and $\rm 12+\log(O/H) = 6.81_{-0.04}^{+0.04}~\rm dex$ (1.3\% $\rm Z_{\odot}$). We identify a rare outlier population of 24 galaxies with high N/O ratios at low metallicity, reminiscent of galaxy abundances observed in the early Universe. We find the Ne/O ratio is constant at low metallicity but increases gradually at $\rm 12+log(O/H) > 8.105\pm0.004$ dex. We show that the S/O and Ar/O abundance ratios are strongly correlated, consistent with the expected additional Type Ia enrichment channel for S and Ar. In this work we present an initial survey of the key properties of the sample, with this dataset serving as a foundation for extensive future work on galaxy abundances at low redshift.

Figures

Figures reproduced from arXiv: 2601.02463 by A. de la Macorra, A. Kremin, A. Meisner, A. Saintonge, B. Andrews, B. A. Weaver, B. Dey, C. Poppett, D. Bianchi, D. Brooks, D. Schlegel, D. Scholte, D. Sprayberry, E. Gazta\~naga, E. Sanchez, F. Cullen, F. J. Castander, F. Prada, G. Gutierrez, G. Rossi, G. Tarl\'e, H. Zou, I. P\'erez-R\`afols, J. Aguilar, J. E. Forero-Romero, J. Moustakas, J. Silber, J. Sui, K. Douglass, K. Z. Arellano-Cordova, L. Le Guillou, M. Landriau, O. Lahav, P. Doel, P. Martini, R. Joyce, R. Miquel, S. Ahlen, S. Ferraro, S. Gontcho A Gontcho, T. Cheng, T. Claybaugh, T. M. Stanton, W. J. Percival, Z. Shao.

Figure 1
Figure 1. Figure 1: Figure of an example DESI spectrum of DESI J031.5272+08.5595 with the fitted FastSpecFit (Moustakas et al. 2023a) model. The spectrum is shown in black with uncertainties in the flux measurements shown by the grey band. The fitted model is shown in red. We highlight the fitted emission lines in each panel with pink vertical bands and the names of the fitted lines. In the bottom panel we show five inset fig… view at source ↗
Figure 2
Figure 2. Figure 2: The redshift distribution of the galaxies with temperature measure￾ments in our sample (grey). The vertical lines show the maximum redshift where the 𝑇e can be determined based on the listed ionic species. The coloured histogram outlines in matching colours show the measurement distribution of electron temperatures of each ion [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: The histograms of the electron temperature measurements de￾rived from the auroral emission lines of different ions. The red dashed lines show the median electron temperature measured using each auroral line. The [Oiii]𝜆4363 auroral line (corresponding to 𝑇e (O ++)) is brightest at high temperatures, the [Siii]𝜆6312 emission line (correcponding to 𝑇e (S ++)) is brightest at intermediate temperatures and 𝑇e … view at source ↗
Figure 4
Figure 4. Figure 4: The electron temperature relation between the high-ionisation zone, 𝑇e (O ++), and the intermediate-ionisation zone, 𝑇e (S ++). The red line shows the best fit relation derived from our observations. The shaded region shows the 1𝜎 uncertainty in the relation. The total scatter in the relation is 𝜎tot(S ++) = 1700 K and the intrinsic scatter is 𝜎int(S ++) = 900 K. The total scatter in 𝑇e (O ++) is 𝜎tot(O ++… view at source ↗
Figure 5
Figure 5. Figure 5: The electron temperature relation between the high-ionisation zone, 𝑇e (O ++), and the low-ionisation zone, 𝑇e (O + ). The red line shows the best fit relation derived from our observations. The shaded region shows the 1𝜎 uncertainty in the relation. The total scatter in the relation is 𝜎tot(O + ) = 2100 K and the intrinsic scatter is 𝜎int(O + ) = 1700 K. The total scatter in 𝑇e (O ++) is smaller at 𝜎tot(O… view at source ↗
Figure 7
Figure 7. Figure 7: A compilation of the electron temperature relations between measurements from different ions. The red lines show the best fit relations derived from our observations. The shaded regions show the 1𝜎 uncertainties in the relations. All data points are coloured by the Gaussian kernel density of the plotted distribution. This is visible in the number of high 𝑇e (N + ) outliers in the relevant panels of [PITH_… view at source ↗
Figure 8
Figure 8. Figure 8: The ionic abundance ratios as a function of the degree of ionisation, defined as O ++/O, shown together with the relations for ionisation correction factors by Izotov et al. (2006), Pérez-Montero et al. (2007), Dors et al. (2013) and Amayo et al. (2021) as indicated by the legend. Due to systematic evolution of the N/O ratio the data is not expected to coincide with the plotted ICFs in the top-left panel a… view at source ↗
Figure 9
Figure 9. Figure 9: Oxygen abundances as a function of electron temperature of the high ionisation zone. We show 𝑇e (O ++) (purple squares), for objects where this is measured, and show the converted values of 𝑇e (S ++) (teal diamonds) or 𝑇e (O + ), 𝑇e (N + ) or 𝑇e (S + ) (lime-green circles) using the fiducial temperature relations if the preceding are not available. The data points are shaded by the Gaussian kernel density … view at source ↗
Figure 10
Figure 10. Figure 10: The abundance ratios, log(X/O), versus metallicity for nitrogen (top-left), neon (top-right), sulphur (bottom-left) and argon (bottom-right). The blue lines shows literature relations derived by Izotov et al. (2006), Andrews & Martini (2013), Nicholls et al. (2017) and Berg et al. (2012, 2019). The orange lines show the predicted relations from chemical evolution models for the Solar neighbourhood, Milky … view at source ↗
Figure 11
Figure 11. Figure 11: The mass-metallicity relation (left), the mass-N/O relation (middle) and the star formation main sequence (right). The data points are coloured by the Gaussian kernel density of the plotted distribution. Typical uncertainties are shown by the black error bars in the bottom-right corner of each panel. The red data with error bars show the median measurements and 16th to 84th percentiles at fixed stellar ma… view at source ↗
Figure 12
Figure 12. Figure 12: The S/O ratio as a function of the Ar/O ratio. The dashed black line shows the expected relation with unity slope corrected for the relative difference in abundance between sulphur and argon as measured through the median values of our sample: log(Ar/O) = log(S/O) − 0.78 dex. The strong correlation between the two ratios is expected due to the similar production channels of sulphur and argon, this is also… view at source ↗

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Cited by 3 Pith papers

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