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arxiv: 2606.03753 · v1 · pith:33DO3OXZnew · submitted 2026-06-02 · 🌌 astro-ph.CO · astro-ph.GA

The impact of source and survey modelling on the connection between [O III] emitters and Ly α forest transmission at z ~ 6

Luke Conaboy , James S. Bolton , Laura C. Keating , Martin G. Haehnelt , Girish Kulkarni , Ewald Puchwein This is my paper

Pith reviewed 2026-06-28 08:28 UTC · model grok-4.3

classification 🌌 astro-ph.CO astro-ph.GA
keywords [O III] emittersLyα forest transmissioncross-correlationJWST surveysionising sourcesz~6intergalactic mediummock catalogues
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The pith

Mock surveys incorporating JWST geometry produce large scatter in [O III]-Lyα cross-correlations that statistically matches observations at z~6.

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

The paper builds an empirical model that links dark matter haloes to the observed population of [O III] emitters while folding in the exact geometry and depth of JWST surveys to generate realistic mock catalogues. These mocks are then compared against measured galaxy clustering and both the one- and two-dimensional cross-correlations with Lyα forest transmission. The resulting scatter in the mock cross-correlation measurements is large enough to produce a statistically acceptable match to the data, even though the one-dimensional correlation peaks at a comoving scale roughly 10 cMpc smaller than observed. This scatter leads to the conclusion that present galaxy-IGM observations lack the power to exclude a wide variety of ionising source models. The authors note that larger observational samples and simulations in volumes exceeding 250 cMpc will be needed to make further progress.

Core claim

By constructing an empirical model that connects haloes with the observed population of [O III] emitters and incorporates the geometry and depth of the JWST surveys into mock galaxy survey catalogues, the large scatter in the mock survey measurements of the cross-correlation enables a statistically good match to the observational data, albeit the peak of the one dimensional correlation in the mocks occurs at a scale ≈10 cMpc below that observed.

What carries the argument

An empirical model that connects haloes with the observed population of [O III] emitters and incorporates the geometry and depth of the JWST surveys into mock galaxy survey catalogues.

If this is right

  • The large scatter in mock cross-correlation measurements allows a statistically good match to the observed data.
  • The peak of the one-dimensional correlation in the mocks occurs at a scale ≈10 cMpc smaller than observed.
  • Current galaxy-IGM observations may struggle to rule out a broad range of ionising source models.
  • Further progress requires increased observational sample sizes and simulations performed in box sizes >250 cMpc that use a variety of source models.

Where Pith is reading between the lines

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

  • If the scale offset in the correlation peak persists in larger volumes, it may point to missing large-scale modes or source clustering physics rather than survey geometry alone.
  • The limited constraining power identified here suggests that combining the [O III]-Lyα cross-correlation with other high-redshift probes could still be needed to narrow the range of viable reionisation histories.
  • Larger simulation boxes might also reduce cosmic variance in the mocks, potentially tightening the allowed range of ionising source models even before new observations arrive.

Load-bearing premise

The empirical model that connects haloes with the observed population of [O III] emitters and incorporates the geometry and depth of the JWST surveys into mock galaxy survey catalogues is sufficiently accurate to produce representative cross-correlation statistics.

What would settle it

A future observational data set with substantially larger sample size that shows the one-dimensional cross-correlation peak consistently at the observed scale (rather than the mock scale) or exhibits significantly smaller scatter would falsify the claim that current data cannot distinguish among ionising source models.

Figures

Figures reproduced from arXiv: 2606.03753 by Ewald Puchwein, Girish Kulkarni, James S. Bolton, Laura C. Keating, Luke Conaboy, Martin G. Haehnelt.

Figure 1
Figure 1. Figure 1: — Simulated UV luminosity functions (left panel, lines), with observational data from Matthee et al. (2023) (grey hexagons). We also show the corresponding [O iii]λ5008 luminosity functions (right panel, lines) with observational data from Matthee et al. (2023) (grey hexagons), Sun et al. (2023) (grey diamonds), and Meyer et al. (2025) (grey triangles). The simulated luminosity functions are shown every ∆z… view at source ↗
Figure 2
Figure 2. Figure 2: — Simulated [O iii]λ5008 volume-averaged projected autocorrelation functions (solid) for all haloes in the catalogue, compared to observational results from Eilers et al. (2024) (grey squares) and Huang et al. (2026) (grey triangles), both covering the redshift range 5.3 < z < 7.0 and using the same binning (al￾though for clarity, we shift the Huang et al. (2026) points slightly left and the Eilers et al. … view at source ↗
Figure 3
Figure 3. Figure 3: ) is well-fit by a Gaussian with mean ⟨MUV⟩ = −19.7 and standard deviation σMUV = 0.7. For each of the five quasar sightlines in the ASPIRE survey we there￾fore draw [O iii] emitters from this Gaussian such that the mean number of [O iii] emitters in a typical ASPIRE￾like realisation ⟨N[O iii]⟩ is similar to that in Kakiichi et al. (2025). At z = 6.4, 6.0, and 5.6 we find ⟨N[O iii]⟩ = 7.2, 8.8, and 10.2, c… view at source ↗
Figure 4
Figure 4. Figure 4: — The probability distribution of halo masses used in the calculation of the [O iii] emitter-Ly α cross-correlation at z = 6 (see [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: — The galaxy-Ly α transmission cross correlation at z = 6.4, 6.0 and 5.6 (top, middle and bottom panels) for our full forward model. Solid curves indicate the mean, and the violin plots indicate the distribution of δF within each r bin from 1024 ASPIRE-like realisations using kernel density estimation. Note that at z = 6.4, some of the bins extend to larger values of δF than shown here but, to preserve dyn… view at source ↗
Figure 6
Figure 6. Figure 6: — The relation between galaxy surface density and Ly α forest effective optical depth at z = 5.6. The galaxy surface density is measured in a 28 h−1 cMpc window, and the Ly α forest effective optical depth in a 50 h−1 cMpc window. The median relation for the mock [O iii] sample is shown by the solid curve, along with the 68 per cent (dark band) and 95 per cent (light band) ranges. The dotted curves show th… view at source ↗
Figure 7
Figure 7. Figure 7: — Fraction of segments in each τ 50 eff bin that are, on average, underdense (⟨∆⟩ < 1, pale pink), and both underdense and hot (⟨T⟩ > T0, where T0 is the temperature at ∆ = 1, pink), where the average is calculated over the entire segment. We also show the fraction of segments that contain at least one neutral island, defined as a contiguous region with xH i > 0.5 of extent ≥ 2 cMpc (blue). The fraction re… view at source ↗
Figure 8
Figure 8. Figure 8: — Projected autocorrelation function χV of [O iii] emit￾ters at z = 6 (top panel) for our fiducial duty cycle ∆t = 50 Myr (black), as well as for duty cycles of ∆t = 25, 100 and 200 Myr (blue, purple and pink, respectively), along with observational con￾straints due to Eilers et al. (2024) (grey squares) and Huang et al. (2026) (grey triangles). We also show the ratio of χV for each of these duty cycles to… view at source ↗
Figure 9
Figure 9. Figure 9: — Galaxy–Ly α transmission correlation at z = 6 for our fiducial duty cycle ∆t = 50 Myr (black), as well as for duty cycles of ∆t = 25, 100 and 200 Myr (blue, purple and pink, respectively), along with the distribution from Conaboy et al. (2025) (grey dot￾ted). 10 11 12 13 log10(Mh/M ) 10−4 10−3 0.01 0.1 1 p(log10 Mh) z = 6.0 [PITH_FULL_IMAGE:figures/full_fig_p014_9.png] view at source ↗
Figure 11
Figure 11. Figure 11: — Comparison of χV at z = 6.2 estimated using our fiducial FoF halo catalogue (solid line) and using a rockstar cat￾alogue (dotted line). Also shown are observational constraints due to Eilers et al. (2024) (grey squares) and Huang et al. (2026) (grey triangles). log10(Mh/h−1 M⊙) > 10.5, where this lower mass limit is chosen to reproduce our abundance-matched χV for r⊥ > 1 cMpc. We find that, for r⊥ ≲ 0.4… view at source ↗
Figure 10
Figure 10. Figure 10: — Distribution of halo masses used to compute δF at z = 6 for our fiducial duty cycle ∆t = 50 Myr (black), as well as for duty cycles of ∆t = 25, 100 and 200 Myr (blue, purple and pink, respectively), along with the distribution from Conaboy et al. (2025) (grey dotted). The line styles are as in [PITH_FULL_IMAGE:figures/full_fig_p014_10.png] view at source ↗
read the original abstract

James Webb Space Telescope (JWST) surveys of [O III]-emitting galaxies are offering fresh insight into the connection between galaxies and the intergalactic medium at redshift z ~ 6. Recent measurements of the cross-correlation between [O III]-emitting galaxies and Ly $\alpha$ forest transmission present an apparent challenge to numerical models. Here we improve upon previous theoretical work by constructing an empirical model that connects haloes with the observed population of [O III] emitters and incorporates the geometry and depth of the JWST surveys into mock galaxy survey catalogues. We compare these mocks to recent measurements of [O III] emitter clustering and the one and two dimensional galaxy-Ly $\alpha$ transmission cross-correlation. The large scatter in our mock survey measurements of the cross-correlation enable a statistically good match to the observational data, albeit the peak of the one dimensional correlation in our mocks occurs at a scale $\approx$10 cMpc below that observed. The large scatter implies that, at present, current galaxy-IGM observations may struggle to rule out a broad range of ionising source models. We anticipate that further progress will strongly benefit from increased observational sample sizes, as well as simulations performed in box sizes >250 cMpc that use a variety of source models.

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

0 major / 3 minor

Summary. The manuscript constructs an empirical model mapping dark matter haloes to the observed population of [O III] emitters at z ~ 6, incorporating JWST survey geometry and depth to generate mock galaxy catalogues. These mocks are compared against observational measurements of [O III] emitter clustering as well as the one- and two-dimensional cross-correlations between galaxies and Lyα forest transmission. The central result is that the large scatter present in the mock cross-correlation measurements permits a statistically acceptable match to the data, even though the peak of the one-dimensional correlation function in the mocks is offset by ~10 cMpc relative to the observations; this scatter implies that current galaxy-IGM data have limited power to discriminate among ionising source models. The authors also note that simulations in boxes larger than 250 cMpc will be required for further progress.

Significance. If the empirical halo-to-emitter mapping and survey-mock construction are representative, the work usefully quantifies the role of cosmic variance and survey specifics in high-redshift galaxy-IGM cross-correlations. It supplies a concrete illustration that large scatter can reconcile model and data even when the location of the correlation peak differs, thereby tempering claims about the constraining power of existing observations. The explicit comparison of the same mocks to measured [O III] clustering provides an internal consistency check that strengthens the analysis.

minor comments (3)
  1. [Abstract] Abstract: the statement that the mock 1D peak occurs “at a scale ≈10 cMpc below that observed” would be clearer if the numerical values of both the observed and mock peak locations (with uncertainties) were stated explicitly.
  2. The manuscript would benefit from a short table or paragraph summarising the key parameters of the empirical halo-to-[O III] mapping (e.g., duty cycle, luminosity threshold, scatter) so that readers can immediately assess how many free choices enter the model.
  3. Figure captions (or the text describing the 1D and 2D cross-correlation measurements) should explicitly state the binning scheme and the precise definition of the transmission field used, to facilitate direct reproduction of the reported scatter.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive and accurate summary of the manuscript and for recommending minor revision. No specific major comments were provided in the report.

Circularity Check

0 steps flagged

No significant circularity identified

full rationale

The paper builds an empirical halo-to-[O III] emitter model calibrated against observed galaxy populations and survey geometries, generates mock catalogues, and performs direct statistical comparisons of the resulting galaxy-Lyα transmission cross-correlations against independent external observational datasets. No derivation step reduces by construction to the target correlation via self-definition, fitted parameters renamed as predictions, or load-bearing self-citations; the large-scatter claim is framed as an outcome of the comparison rather than an internal tautology. The modeling choices are presented as necessary inputs for testing against data, with explicit caveats about sample size and box size requirements.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review; no explicit free parameters, axioms, or invented entities are described. The empirical connection between haloes and [O III] emitters is the central modeling step whose details are not provided.

pith-pipeline@v0.9.1-grok · 5797 in / 1180 out tokens · 39853 ms · 2026-06-28T08:28:32.229648+00:00 · methodology

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