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Lyα haloes around faint galaxies at z≥6 are three times smaller than at z~3, and most leave no extended emission even in stacks.

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2026-07-11 09:00 UTC pith:HMGSRCZW

load-bearing objection First sensitivity-matched comparison of low-luminosity LAHs at z≥6 vs z~3 shows a clean factor-of-three size drop and a null high-z stack; the result holds after the paper's own resolution checks. the 2 major comments →

arxiv 2607.05087 v1 pith:HMGSRCZW submitted 2026-07-06 astro-ph.GA

Lyman-alpha haloes in the aftermath of reionisation

Daniil Smirnov , Lutz Wisotzki , Tanya Urrutia , John Pharo , Ramona Augustin , Yucheng Guo , Daria Kozlova , Haruka Kusakabe
show 3 more authors
Jorryt Matthee Ismael Pessa Joop Schaye
This is my paper
classification astro-ph.GA
keywords Lyman-alpha haloesLyman-alpha emittersreionisationcircumgalactic mediumMUSEhigh-redshift galaxiessurface-brightness dimming
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 compares Lyman-alpha haloes around low-luminosity Lyman-alpha emitters at z≥6 with a carefully matched sample at z~3. The data are chosen so that the intrinsic surface-brightness sensitivity is the same after cosmological dimming is removed. Individual extended emission is found around only a third of the high-redshift objects, and those haloes are typically three times more compact than their lower-redshift counterparts. Stacking the non-detections recovers a clear, large halo at z~3 but no extended signal at all at z≥6. The high-redshift lines are also ~2.5 times narrower. The authors argue that either residual neutral gas after reionisation scatters most photons out of detectability, or that halo sizes simply grow in step with their host galaxies and dark-matter haloes. Either way, the circumgalactic Lyman-alpha glow of ordinary star-forming galaxies looks radically different just after reionisation ends.

Core claim

When samples of faint Lyman-alpha emitters are matched in intrinsic surface-brightness sensitivity, luminosity and stellar mass, the typical exponential scale lengths of their Lyman-alpha haloes at z≥6 are three times smaller than at z~3. Stacking the individually undetected objects yields a highly significant extended halo at low redshift but no trace of extended emission at high redshift; the high-redshift lines are also ~2.5 times narrower.

What carries the argument

Intrinsic surface-brightness matching (SBlim,Lyα ∝ σ_eff(λ)/(1+z)^4) that equalises the detectability of intrinsically identical haloes across redshift, allowing a direct comparison of exponential scale lengths, halo flux fractions and stacked profiles.

Load-bearing premise

That correcting the effective noise for cosmological dimming fully equalises the ability to detect identical intrinsic haloes, so residual sensitivity, PSF or angular-size biases cannot produce the observed size and stacking differences.

What would settle it

A new set of MUSE or equivalent integral-field observations that reaches the same intrinsic surface-brightness limit at both redshifts and recovers either large high-z haloes or a clear stacked high-z halo of scale length comparable to the z~3 sample would falsify the claimed size dichotomy.

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

If this is right

  • Most faint LAEs at z≥6 either lack Lyman-alpha haloes or host only very compact ones, so deep stacks will not recover the large haloes seen at lower redshift.
  • The two main drivers of LAE detectability—halo size and line width—evolve strongly, altering the selection function and therefore the observed Lyman-alpha luminosity function near the end of reionisation.
  • Halo scale length relative to virial radius remains roughly constant (~0.16), linking the growth of the scattering medium directly to dark-matter halo assembly if coevolution is the dominant driver.
  • If reionisation is responsible, detectable high-z LAHs preferentially flag galaxies that sit inside larger or more highly ionised bubbles.

Where Pith is reading between the lines

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

  • The same intrinsic-sensitivity matching applied across the full MUSE redshift range (z~3–6) would decide whether halo sizes evolve smoothly with galaxy size or jump only near reionisation.
  • Narrow high-z lines together with compact (or absent) haloes imply that the photons we detect have experienced less resonant scattering than at lower redshift, offering a new handle on local ionised-bubble size.
  • If halo size tracks virial radius, future intensity-mapping experiments that resolve the diffuse Lyman-alpha background should see a corresponding change in the small-scale power spectrum between z~6 and z~3.

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

2 major / 5 minor

Summary. The paper compares Lyα haloes (LAHs) around low-luminosity LAEs (L_Lyα ≲ 10^42 erg s^{-1}) at z ≥ 6 (18 objects from the MXDF) with a reference sample at z ∼ 3.2 (90 objects from MUSCATEL-SF A2744), constructed so that the samples share the same intrinsic surface-brightness sensitivity after the (1 + z)^4 cosmological-dimming correction (Eq. 1, Fig. 2). Extended emission is detected around 6/18 high-z LAEs (more than doubling the known sample at z ≥ 6) versus 40/90 at low z. The high-z exponential scale lengths are typically a factor of ∼3 smaller; stacking the individually undetected objects recovers a highly significant extended halo at z ∼ 3 but none at z ≥ 6. Lyα line widths are also ∼2.5 times narrower at high z. Two interpretations are discussed: reionisation-driven scattering losses that leave only compact emission, or coevolution of LAHs with host-galaxy sizes and dark-matter haloes.

Significance. If the factor-of-three size difference and the null high-z stack hold, the result supplies the first carefully controlled statistical view of faint LAHs in the late reionisation epoch and tightens constraints on both CGM evolution and the topology of ionised bubbles. Strengths include the explicit matching of intrinsic SB sensitivity, the empty-field self-calibration of the p_0 = 0.05 detection threshold, the doubling of known individual z ≥ 6 LAHs, and the quantitative appendices on upper limits (Appendix B) and residual PSF/D_A biases (Appendix C). The work is purely observational, free of circular parameter reuse, and yields a clear, falsifiable contrast between the two physical scenarios.

major comments (2)
  1. §4.3 and Appendix C: The residual resolution + angular-diameter-distance bias is quantified by re-projecting the six high-z GALFIT models to z = 3.2 under MUSCATEL-SF conditions, recovering only the three largest (r_s,H > 2 kpc). This demonstrates that the bias cannot manufacture the absence of large high-z haloes or the null stack of the 12 non-detections. However, the main text still quotes a clean factor-of-three mean ratio and a KS p = 0.0008 without folding the Appendix C selection function into the reported distributions or the KS statistic. A short Monte-Carlo or re-weighted comparison that includes the factor ∼2 change in minimum detectable size would make the central claim fully robust against the paper’s own weakest assumption.
  2. §2.3 and §6.1: Seven of the 18 high-z LAEs lack JWST continuum counterparts, so stellar masses and SFRs are unavailable for them. The Bhattacharyya-distance comparison of M⋆ and SFR distributions (and the claim that sample differences cannot explain the halo-size change) is therefore performed only on the 11 objects with counterparts. Because the non-detections are among the faintest systems, it remains possible that the full high-z sample is systematically lower-mass than the low-z sample. Either assign conservative upper limits on M⋆ for the continuum-undetected objects or demonstrate that the scale-length and stacking results are unchanged when the comparison is restricted to the UV-detected subset.
minor comments (5)
  1. Table 2 caption: “measuredz>Lyαhalo” is missing spaces and a greater-than sign; correct to “measured z ≥ 6 Lyα halo o”.
  2. Fig. 3 caption: “F ourth column” contains a stray space; also the p0 values printed on the panels would be clearer if given to consistent precision.
  3. §2.2: The MUSCATEL survey description still contains the placeholder “XXXXXXXX, in preparation”; replace with the actual reference or “in prep.” once available.
  4. §5 and Fig. 7: The predicted virial FWHM bars rely on the Behroozi et al. (2013) SMHM relation extrapolated to low masses and high z; a brief note on the systematic uncertainty of that conversion would help the reader gauge the “little evidence for further broadening” statement.
  5. Appendix A Fig. A.1: The three panels share the same y-axis label “SB(z = 3.2)”; adding a short note that the high-z points have already been scaled by the dimming factor would avoid confusion.

Circularity Check

0 steps flagged

No significant circularity: purely observational comparison of matched samples with standard exponential+continuum fits and self-calibrated detection; no predictions forced by construction or load-bearing self-citation chains.

full rationale

The paper's central results (factor-of-three smaller LAH scale lengths at z≥6, null high-z stack of non-detections vs. significant low-z stack, narrower line widths) are direct measurements from MUSE NB images and spectra of two samples constructed to share the same intrinsic SB sensitivity via Eq. 1 and Fig. 2. Detection uses a conventional p0=0.05 threshold self-calibrated on empty-field χ^{2} distributions (Sect. 3.2), not tuned to the result. Halo modelling (Sect. 4.1) adopts the literature-standard sum of UV-continuum template plus exponential, with free parameters fitted to the data and reported; no fitted parameter is re-used to 'predict' a related observable. Stacking (Sect. 4.3, App. A) and upper limits (App. B) are likewise empirical. Prior MUSE results (LW16, FL17) by overlapping authors are cited only for methodological continuity and comparison of lower-z distributions, not as uniqueness theorems or load-bearing premises that force the high-z outcome. Appendix C quantifies residual PSF/DA biases via mocks without circular reuse. The derivation chain is therefore self-contained observational analysis against external data, with no reduction of claims to their own inputs by definition or fit.

Axiom & Free-Parameter Ledger

3 free parameters · 4 axioms · 0 invented entities

The central empirical claim rests on standard cosmological surface-brightness dimming, the assumption that UV continuum morphology traces the unscattered Lyα core, a conventional p0=0.05 detection threshold, and the Behroozi stellar-to-halo mass relation used only for secondary line-width interpretation. No new physical entities are introduced; free parameters are limited to conventional fit choices.

free parameters (3)
  • p0 detection threshold = 0.05
    Fixed at 0.05 for declaring a halo detection after self-calibration on empty fields; conventional but still a choice that sets the individual detection fractions.
  • narrow-band spectral width = ~11.25 Å
    Manually chosen ~9 MUSE pixels (11.25 Å) per object to capture most of the red peak while excluding blue peaks; affects total flux and SB profiles.
  • exponential halo scale length rs,H and flux fraction fH = median ~1.5–2 kpc (z≥6) vs ~5 kpc (z~3)
    Free parameters of the two-component GALFIT model fitted to each detected NB image; the reported size difference is the distribution of these fitted values.
axioms (4)
  • domain assumption Cosmological surface-brightness dimming scales exactly as (1+z)^4 and can be inverted to match intrinsic SB sensitivity between redshifts (Eq. 1).
    Standard FLRW result; used to select the MUSCATEL-SF comparison sample.
  • domain assumption The UV continuum spatial distribution, after PSF convolution, is an adequate null model for the unscattered Lyα core.
    Standard in LAH literature (LW16, FL17); invoked throughout the detection procedure in §3.
  • standard math ΛCDM cosmology with H0=70, Ωm=0.3, ΩΛ=0.7 for converting angular to physical scales.
    Stated in §1; used for all kpc conversions.
  • domain assumption Behroozi et al. (2013) stellar-mass–halo-mass relation plus Evrard et al. (2008) virial calibration give indicative 1-D velocity dispersions.
    Used only for secondary comparison of observed vs predicted line widths in §5; not required for the size claim.

pith-pipeline@v1.1.0-grok45 · 36620 in / 2851 out tokens · 27767 ms · 2026-07-11T09:00:38.335758+00:00 · methodology

0 comments
read the original abstract

We present a comparative study of Ly$\alpha$ haloes (LAHs) around low-luminosity (L$_{\mathrm{Ly}\alpha}\lesssim 10^{42}$ erg s$^{-1}$) Ly$\alpha$-emitting galaxies (LAEs) at very high redshifts $z\geq6$ and a reference sample at $z\sim 3$ covering a similar Ly$\alpha$ luminosity and host galaxy stellar mass range. Using data from the Multi-Unit Spectroscopic Explorer (MUSE) at the ESO VLT, we extracted the samples such that at the different redshifts we obtain the same intrinsic surface brightness sensitivity, accounting for cosmological dimming. We detect extended Ly$\alpha$ emission around 6 out of 18 high-$z$ LAEs in the MUSE eXtremely Deep Field (MXDF), more than doubling the number of known such objects at $z\geq6$. We obtain an only slightly higher individual LAH detection fraction of 40% among the lower redshift comparison sample. Yet the typical exponential scale lengths at $z\geq6$ are three times smaller than those at $z\sim3$. Stacking the LAEs with undetected haloes gives again drastically different results for the two samples, with a highly significant halo detection at $z\sim 3$ but no trace of extended Ly$\alpha$ emission at $z\geq6$. We also find the Ly$\alpha$ spectral line widths of the high-$z$ sample to be $\sim$2.5 smaller in comparison to the lower redshift objects. We discuss the potential mechanisms driving such strong changes. In a reionisation-driven scenario the higher neutral fraction in the intergalactic and circumgalactic media might lead to substantial scattering losses of escaping Ly$\alpha$ radiation, leaving detectable only emission from the vicinity of the star-forming regions. In an alternative scenario the LAH properties might be linked more closely to the evolution of their host galaxies than previously thought.

Figures

Figures reproduced from arXiv: 2607.05087 by Daniil Smirnov, Daria Kozlova, Haruka Kusakabe, Ismael Pessa, John Pharo, Joop Schaye, Jorryt Matthee, Lutz Wisotzki, Ramona Augustin, Tanya Urrutia, Yucheng Guo.

Figure 1
Figure 1. Figure 1: Top: Spatial distribution of LAEs from high and lower redshift samples in their respective fields. The dashed and solid lines in the top left panel show the MXDF 30- and 140-hour exposure time iso￾contours. Bottom: Examples of Lyα spectra from both samples. The dashed vertical lines indicate the spectral bandwidth used to extract the pseudo-narrowband images used in the analysis. The thin black lines show … view at source ↗
Figure 2
Figure 2. Figure 2: Intrinsic (redshift-corrected) surface brightness sensitivity limit SBlim, Lyα as a function of wavelength (Lyα redshift) for MUSE dat￾acubes from different surveys as indicated in the legend (see text for references). The red horizontal histogram on the left shows the distri￾bution of SBlim, Lyα of our z ≥ 6 sample, and the red dashes mark the observed Lyα wavelengths of the objects in that sample. texp =… view at source ↗
Figure 3
Figure 3. Figure 3 [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Comparison of main LAH parameters for the z ∼ 3 and z ≥ 6 samples. The z ∼ 3 objects are shown as blue squares, the z ≥ 6 objects as red hexagons. The open markers in￾dicate objects where the halo was forced to be circular in the fit. In the left panel we plot halo scale lengths against halo flux fractions, in the middle panel against halo axis ratios. The right panel shows the marginalised histograms of o… view at source ↗
Figure 5
Figure 5. Figure 5: Gallery of the six individually detected z ≥ 6 Lyα haloes. Top row: Lyα narrow band images overlayed with smoothed SB contours (solid blue line) outlining emission from the core and the extended halo with values indicated in the color bar on top. Red contours show the F115W images of the assigned UV counterparts at JWST resolution (their absence indicates no counterpart). Fore- and background objects from … view at source ↗
Figure 6
Figure 6. Figure 6: contrasts the resulting median-stacked Lyα SB pro￾files for the two samples. For this comparison we scaled the SB values of the z ≥ 6 stack by a factor of 9.12 to their equivalent values at redshift z = 3.2 (the median redshift of the MUSCA￾TEL sample), thus approximately correcting for cosmological SB dimming. More details on the stacking results that include also the detected LAH objects are provided in … view at source ↗
Figure 7
Figure 7. Figure 7: compares the line width distributions of the LAEs in our two samples. Most of the lines at both high and low red￾shift are resolved, although some of them only marginally. Only ∼ 20% of the FWHM values fall below the LSF resolution, im￾plying that their widths cannot be adequately constrained. The figure also shows the FWHM distributions for only the objects with individually detected haloes. We confirm th… view at source ↗
Figure 8
Figure 8. Figure 8: Measured Lyα scale lengths as a function of redshift. The individually detected haloes from this study are shown as small squares (z ∼ 3.2) and hexagons (z ≥ 6), while sample median values are given by the big dark markers. These are compared to results from previous MUSE observations (LW16, FL17) and from stacking (Momose et al. 2014 – RM14, Wu et al. 2020 – JW20) as resolved in the legend, again with sma… view at source ↗

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Reference graph

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