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arxiv: 2604.18730 · v1 · submitted 2026-04-20 · 🌌 astro-ph.GA

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New constraints on stellar feedback through [O III] emission: interpreting ALMA and JWST observations with SPICE simulations

Benedetta Casavecchia , Aniket Bhagwat , Benedetta Ciardi , Celine Peroux , Tiago Costa
Authors on Pith no claims yet

Pith reviewed 2026-05-10 03:41 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords stellar feedback[OIII] emissionhigh-redshift galaxiessupernova prescriptionsmetal enrichmentluminosity functionscosmological simulationsEpoch of Reionization
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The pith

Bursty supernova feedback produces fewer bright [OIII] emitters than smooth feedback by z=5.

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

The paper introduces a post-processing pipeline to calculate [OIII] line emission from radiation-hydrodynamical simulations that test three different supernova feedback prescriptions. It finds that the bursty supernova model ionizes gas efficiently yet enriches galaxies with metals less effectively than the smooth model, yielding fewer luminous [OIII] sources at high redshift while both the bursty and hypernova models suppress the bright end of the luminosity function. Emission arises mainly from gas that is simultaneously shock-heated and radiatively ionized, with links to neutral gas content and the mass-metallicity relation. This matters for interpreting new ALMA and JWST detections of [OIII] at z greater than 6, because the line serves as a direct probe of how stellar feedback shapes early galaxy growth and metal distribution.

Core claim

We have developed a post-processing pipeline that implements a sub-grid model for [OIII] line emission within the SPICE radiation-hydrodynamical simulations exploring three supernova feedback prescriptions: bursty-sn, smooth-sn, and hyper-sn. [OIII] emission predominantly originates from gas that is both shock-heated and radiatively ionized. The bursty-sn model efficiently ionizes gas but enriches galaxies less effectively by z = 5, leading to fewer bright [OIII] emitters compared to the smooth-sn model, while both bursty-sn and hyper-sn produce suppressed luminosity functions. Spatially resolved maps show that smooth-sn tends to generate more compact galaxies and slightly higher V/σ values,

What carries the argument

Post-processing pipeline for [OIII] line emission that applies a sub-grid model of combined shock heating and radiative ionization to the output of SPICE simulations run with three distinct supernova feedback prescriptions.

If this is right

  • [OIII] emission acts as a sensitive tracer of stellar feedback at high redshift.
  • Bursty and hypernova models both suppress the bright end of the [OIII] luminosity function relative to smooth feedback.
  • Smooth feedback produces more compact galaxies with modestly higher V/σ ratios, though substantial overlap remains between models.
  • The correlation between neutral gas fraction and [OIII] luminosity differs across feedback prescriptions.
  • Observations must reach fainter luminosities to capture the strongest effects of feedback on [OIII] emission.

Where Pith is reading between the lines

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

  • If the models are correct, wide-field JWST [OIII] surveys at z greater than 6 could discriminate among supernova feedback implementations used in galaxy formation simulations.
  • The significant overlap in morphological and kinematic properties suggests that multi-line or spatially resolved data will be required to break degeneracies between feedback models.
  • The same post-processing approach could be applied to other rest-frame optical or far-infrared lines to test consistency of the inferred feedback effects.

Load-bearing premise

The sub-grid model for [OIII] line emission accurately represents the combined effects of shock heating and radiative ionization across unresolved scales in the simulations.

What would settle it

Comparison of the predicted [OIII] luminosity functions at z approximately 5 to 7 from each feedback model against the number counts of bright emitters measured in JWST or ALMA surveys; mismatch at the bright end would falsify the differential effect of bursty versus smooth feedback.

Figures

Figures reproduced from arXiv: 2604.18730 by Aniket Bhagwat, Benedetta Casavecchia, Benedetta Ciardi, Celine Peroux, Tiago Costa.

Figure 1
Figure 1. Figure 1: Maps of surface brightness in [O iii] integrated along the line of sight at 5008 Å (top row) and 88 𝜇m (bottom row) for the most massive galaxy at 𝑧 = 7. The first column shows the map for the bursty-sn model, the second for hyper-sn, and the third for smooth-sn. In each panel, the insets in the bottom-right corner display the velocity field maps derived from the luminosities at 5008 Å (top) and 88 𝜇m (bot… view at source ↗
Figure 2
Figure 2. Figure 2: Temperature–density diagram of gas cells in the most massive galaxy at 𝑧 = 5, for the bursty-sn (top panel) and smooth-sn (bottom panel) models. The 2D distribution is color-coded by the sum of intrinsic optical [O iii] luminosities in each density–temperature bin. The plot reveals a multiphase interstellar medium, structured as follows: diffuse, hot gas pro￾duced by stellar feedback (a); shocked gas (b); … view at source ↗
Figure 3
Figure 3. Figure 3: Contribution from each gas phase to the total intrinsic optical [O iii] luminosity, at redshifts 𝑧 = 10, 7, and 5. Red, green, and blue bars represent results from the bursty-sn, hyper-sn, and smooth-sn feedback models, respectively. Following the notation introduced in [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: The left y-axis shows the gas metallicities (dots), while the right y-axis indicates metallicities expressed in terms of [O/H] (crosses). Solid lines show the optical [O iii] luminosity-weighted mean relations in bins of stellar mass. Red, green, and blue points correspond to galaxies in the bursty-sn, hyper-sn, and smooth-sn feedback models, respectively. Observational estimates from ALMA and JWST are sho… view at source ↗
Figure 5
Figure 5. Figure 5: Dust-corrected luminosity functions of [O iii] at 𝑧 = 10, 7, and 5 for the bursty-sn (red), hyper-sn (green), and smooth-sn (blue) feedback models. Solid and dashed lines show median values for the emission at 5008 Å, and 88 𝜇m, respectively. Black points represent JWST observational constraints for the 5008 Å LFs (Matthee et al. 2023; Meyer et al. 2024; Wold et al. 2025). For both transitions, the smooth-… view at source ↗
Figure 6
Figure 6. Figure 6: Dust-corrected 𝐿[O iii] at 5008 Å (top) and 88 𝜇m (bottom) as a function of the neutral gas fraction within the virial radius for galaxies at 𝑧 = 10 (left) and 𝑧 = 5 (right) in the bursty-sn (red), hyper-sn (green), and smooth-sn (blue) models. Contours enclose 50% and 80% of the data, while points indicate individual galaxies outside these contours. The gray-shaded areas mark the region where galaxies hav… view at source ↗
Figure 8
Figure 8. Figure 8: Redshift evolution of the 𝐿[O III],5008 Å half-light radius, for the bursty-sn (red), hyper-sn (green) and smooth-sn (blue) stellar feedback models. Each point corresponds to the luminosity-weighted median value, and the error bars represent the 16th and 84th percentiles of the distribution. The top and bottom panels display the results for galaxies with 106 M⊙ ≤ 𝑀★ ≤ 108 M⊙ and 𝑀★ > 108 M⊙, respectively. … view at source ↗
Figure 7
Figure 7. Figure 7: Dust-corrected 𝐿[O iii] as a function of gas metallicity at 𝑧 = 10 (top), 𝑧 = 7 (middle) and 𝑧 = 5 (bottom) for the bursty-sn (red), hyper-sn (green), and smooth-sn (blue) models. Lines indicate the median luminosi￾ties for the 5008 Å (solid) and the 88 𝜇m (dashed) transition, while shaded regions represent the 16th–84th percentile range around the medians. Stars indicate single galaxies in metallicity bin… view at source ↗
Figure 9
Figure 9. Figure 9: Half light radius 𝑅1/2 as a function of [O iii] luminosity at 5008 Å. The solid lines represent the median values for bursty-sn (red), hyper-sn (green) and smooth-sn (blue), the shaded areas are the 16th and 84th per￾centiles, while the stars refers to individual galaxies in bins with fewer than four objects. 𝑅1/2 increases with [O iii] luminosity in bursty-sn, decreases in smooth-sn, and shows no clear tr… view at source ↗
Figure 10
Figure 10. Figure 10: Redshift evolution of luminosity weighted 𝑉/𝜎 for galaxies with 106 M⊙ ≤ 𝑀★ ≤ 108 M⊙ (top panel) and 𝑀★ > 108 M⊙ (bottom). Solid lines displays the median values for the bursty-sn (red), hyper-sn (green) and smooth-sn (blue) supernova feedback models, while the shaded areas indicate the 16th and 84th percentiles. Grey points represent a compilation of ALMA and JWST observations based on ionized gas traced… view at source ↗
read the original abstract

ALMA and JWST have recently detected emission lines from the interstellar medium of star-forming galaxies during the Epoch of Reionization, reaching redshifts up to z = 14. Among these, [OIII] lines provide a powerful diagnostic of metal enrichment, gas ionization, and the impact of stellar feedback in galaxies at z > 6. Modeling this emission in cosmological simulations is challenging due to the wide range of spatial scales and physical processes involved. To address this, we have developed a post-processing pipeline that implements a sub-grid model for [OIII] line emission within the SPICE radiation-hydrodynamical simulations. These simulations explore three supernova feedback prescriptions: bursty-sn, smooth-sn, and the hypernova-based hyper-sn. We investigate how these feedback models affect metal enrichment, the neutral gas fraction, and the size and morphology of ionized halos traced by [OIII] emission in both the optical and far-infrared. We find that [OIII] emission predominantly originates from gas that is both shock-heated and radiatively ionized. We also examine the mass-metallicity relation and the correlation between neutral gas fraction and [OIII] luminosity. Our results show that the bursty-sn model efficiently ionizes gas but enriches galaxies less effectively by z = 5, leading to fewer bright [OIII] emitters compared to the smooth-sn model. Both bursty-sn and hyper-sn produce suppressed luminosity functions. Spatially resolved [OIII] emission further indicates that smooth-sn tends to generate more compact galaxies and slightly higher V/{\sigma} values, although there is significant overlap between models. Overall, our findings demonstrate that [OIII] emission is a sensitive tracer of stellar feedback at high redshift and highlight the importance of observations probing fainter luminosities, where feedback effects are strongest.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 1 minor

Summary. The manuscript introduces a post-processing pipeline implementing a sub-grid model for [O III] line emission applied to SPICE radiation-hydrodynamical simulations. These simulations compare three supernova feedback prescriptions: bursty-sn, smooth-sn, and hyper-sn. The analysis focuses on how these models influence metal enrichment, neutral gas fractions, ionized halo morphologies, and [O III] luminosity functions at high redshifts (z > 5). The paper concludes that [O III] emission primarily comes from gas that is both shock-heated and radiatively ionized, that the bursty-sn model ionizes gas efficiently but enriches less effectively leading to fewer bright [O III] emitters by z=5, and that both bursty-sn and hyper-sn produce suppressed luminosity functions compared to smooth-sn.

Significance. Should the sub-grid [O III] model prove reliable, the results offer significant implications for interpreting JWST and ALMA observations of high-redshift galaxies. By linking specific feedback implementations to observable [O III] properties, the work highlights [O III] as a useful tracer for stellar feedback effects during the Epoch of Reionization. The multi-model comparison and emphasis on faint luminosity regimes where feedback impacts are pronounced represent valuable contributions to the field.

major comments (2)
  1. [Post-processing pipeline description] All reported differences between the feedback models in terms of [O III] luminosity functions, ionization efficiency, and enrichment (e.g., bursty-sn producing fewer bright emitters) depend on the sub-grid prescription for [O III] emissivity. The manuscript should include explicit validation tests of this model, such as comparisons to higher-resolution simulations or analytic models of shock and photo-ionization, to confirm that the joint effects are accurately captured rather than being dominated by the approximation.
  2. [Results section on luminosity functions and correlations] The claims of suppressed luminosity functions for bursty-sn and hyper-sn lack accompanying quantitative measures of uncertainty, such as Poisson errors or cosmic variance estimates, and do not discuss how sensitive these suppressions are to the sub-grid parameters. This makes it challenging to evaluate the robustness of the conclusion that these models are distinguishable from smooth-sn.
minor comments (1)
  1. [Discussion of spatially resolved properties] The statement regarding significant overlap between models in V/σ values could be expanded with quantitative metrics or histograms to better illustrate the degree of overlap.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and insightful report. Their comments correctly identify areas where additional validation and quantitative robustness checks would strengthen the manuscript. We address each major comment below and describe the revisions we will implement.

read point-by-point responses

  1. Referee: [Post-processing pipeline description] All reported differences between the feedback models in terms of [O III] luminosity functions, ionization efficiency, and enrichment (e.g., bursty-sn producing fewer bright emitters) depend on the sub-grid prescription for [O III] emissivity. The manuscript should include explicit validation tests of this model, such as comparisons to higher-resolution simulations or analytic models of shock and photo-ionization, to confirm that the joint effects are accurately captured rather than being dominated by the approximation.

    Authors: We agree that the sub-grid [O III] model is foundational to all reported differences and that explicit validation strengthens the interpretation. The model combines standard treatments of collisional excitation in shock-heated gas with radiative ionization, calibrated to local benchmarks and theoretical expectations as outlined in the methods. However, the original manuscript did not present dedicated validation tests against higher-resolution simulations or analytic ionization models. In the revised version we will add a new subsection containing such tests, including direct comparisons to analytic shock and photo-ionization calculations and, where feasible, to results from higher-resolution zoom simulations. These additions will demonstrate that the model captures the joint effects without dominating the differences between feedback prescriptions. revision: yes

  2. Referee: [Results section on luminosity functions and correlations] The claims of suppressed luminosity functions for bursty-sn and hyper-sn lack accompanying quantitative measures of uncertainty, such as Poisson errors or cosmic variance estimates, and do not discuss how sensitive these suppressions are to the sub-grid parameters. This makes it challenging to evaluate the robustness of the conclusion that these models are distinguishable from smooth-sn.

    Authors: We accept that the luminosity-function figures would benefit from explicit uncertainty quantification. The simulations occupy large cosmological volumes, but Poisson errors and cosmic-variance estimates were not reported. In the revised manuscript we will add Poisson error bars to the luminosity-function panels and include a brief assessment of cosmic variance based on the box size and halo statistics. Regarding sensitivity to sub-grid parameters, we will expand the discussion with results from parameter-variation tests performed during model development; these tests show that the main trends (suppression in bursty-sn and hyper-sn relative to smooth-sn) persist across plausible ranges of the key parameters, and we will quantify this robustness explicitly. revision: yes

Circularity Check

0 steps flagged

No circularity: inter-model differences arise from distinct feedback prescriptions

full rationale

The paper executes SPICE radiation-hydrodynamical simulations under three separate supernova feedback prescriptions (bursty-sn, smooth-sn, hyper-sn) and applies the same sub-grid post-processing pipeline to derive [OIII] emissivities. Reported contrasts in metal enrichment, neutral gas fractions, ionized halo sizes, and luminosity functions are direct simulation outputs driven by the differing feedback implementations. No step reduces a claimed prediction to a fitted parameter by construction, invokes a self-citation as the sole justification for a uniqueness claim, or renames an input as an output. The sub-grid [OIII] model is a uniform modeling assumption rather than a definitional loop, leaving the derivation chain self-contained against the simulation inputs.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review provides no explicit list of free parameters, axioms, or invented entities. The work relies on standard assumptions in radiation-hydrodynamical simulations (e.g., sub-grid physics for star formation and feedback) and the validity of the new [OIII] post-processing model.

pith-pipeline@v0.9.0 · 5658 in / 1240 out tokens · 35941 ms · 2026-05-10T03:41:05.756495+00:00 · methodology

discussion (0)

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Reference graph

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