MIGHTEE-HI: Environmental effects of cosmic filaments on extragalactic HI detections in the COSMOS and XMM-LSS fields

Anastasia A. Ponomareva; Bohan Yue; Kristine Spekkens; Maarten Baes; Madalina N. Tudorache; Marcin Glowacki; Matt J. Jarvis; Michalina Maksymowicz-Maciata; Natasha Maddox; Seoyoung Lyla Jung

REVIEW 4 major objections 6 minor 278 references

MIGHTEE-HI: Environmental effects of cosmic filaments on extragalactic HI detections in the COSMOS and XMM-LSS fields

T0 review · 4 major / 6 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read Cosmic filaments measurably alter the neutral hydrogen content of galaxies, draining gas from low-density late-type galaxies while supplying massive early-type galaxies, even after stellar mass, morphology, and local density are controlled.

desk verdict New HI detection fraction trends near filaments are plausible but rest on unshown redshift matching and thin statistics. read the letter →

arxiv 2608.04656 v1 pith:EMKKESMB submitted 2026-08-05 astro-ph.GA

Seoyoung Lyla Jung , Madalina N. Tudorache , Matt J. Jarvis , Michalina Maksymowicz-Maciata , Maarten Baes , Marcin Glowacki , Natasha Maddox , Anastasia A. Ponomareva

show 3 more authors

Kristine Spekkens Tariq Yasin Bohan Yue

This is my paper

classification astro-ph.GA

keywords cosmicfilamentsneutralhydrogenHIdetectionfractiongalaxyenvironmentlarge-scalestructurerampressurestrippingMIGHTEEsurveyevolution

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 asks whether cosmic filaments—the threadlike overdensities of the large-scale galaxy distribution—change how much neutral hydrogen gas galaxies hold. Using 865 optically selected galaxies in two MIGHTEE-HI fields, it measures the fraction detected in HI emission as a function of distance to the nearest filament, while controlling for stellar mass, morphology, and local density. It finds that filament proximity has a measurable, direction-dependent effect: late-type galaxies in low-density environments are less often detected in HI near filaments, while massive early-type galaxies are more often detected there. Because HI is the fuel for star formation, this implies filaments both strip gas and supply gas, with the balance depending on galaxy mass and local environment. If correct, the cosmic web participates directly in setting galaxy gas content, not just the local halo environment.

What carries the argument

The central object is the three-dimensional distance to the nearest cosmic filament, $D_{\rm fil}$, measured from filament skeletons traced by the DisPerSE persistent-topology algorithm applied to DESI spectroscopic galaxies; each galaxy receives a representative $D_{\rm fil}$ from 100 jack-knifed realisations. The statistic that carries the argument is the HI detection fraction, the fraction of optically selected galaxies with an HI source in the MIGHTEE-HI cubes, binned in $D_{\rm fil}$ while holding stellar mass, morphology (Sérsic index plus quiescence), and local density (projected fifth-nearest-neighbour density $\Sigma_5$) fixed. Galaxies at $D_{\rm fil}>5$ Mpc serve as the reference sample, and Monte Carlo binomial tests provide the p-values for deviations.

What would settle it

Compare the HI detection fraction versus D_fil after explicitly matching the redshift distributions of the low- and high-D_fil bins by re-weighting or binning in redshift; if the reduced or enhanced fractions disappear once redshift is matched, the filament signal is a Malmquist-bias artefact. A second check is to stack HI flux at the positions of non-detected galaxies in filament and void samples: identical mean HI content would indicate the detection-fraction difference is a sensitivity or line-width effect rather than genuine gas depletion.

Watch

Extended reading notes

Core claim

We establish that the fraction of DESI galaxies detected in HI emission by MIGHTEE-HI depends on the three-dimensional distance to the nearest DisPerSE-identified cosmic filament even after stellar mass, morphology, and local galaxy number density are controlled. Close to filaments, late-type galaxies at low local density show a lower HI detection fraction than their counterparts more than 5 Mpc from any filament, across all stellar mass bins (cumulative p ≈ 0.03 for $8.5<\log(M_\ast/\mathrm{M}_\odot)<9$ and 0.04 for $\log(M_\ast/\mathrm{M}_\odot)\ge 10$); massive early-type galaxies at low density show the opposite, with the HI detection fraction rising from $14\pm9\%$ beyond 5 Mpc to $50\pm19\%$ within 1.2 Mpc (cumulative p = 0.0119 for $D_{\rm fil}<2.4$ Mpc). We interpret the late-type deficit as ram-pressure stripping and cosmic-web detachment, and the early-type excess as filamentary gas accretion or gas-rich mergers.

Load-bearing premise

The load-bearing premise is that the filament catalogue, built from the same DESI galaxies whose HI detection is analysed, is an unbiased tracer of the true cosmic web and that the D_fil bins being compared have similar redshift distributions, since HI detection falls steeply with redshift and could mimic the observed trends if the bins differ.

Editorial extensions

If this is right

Close to filaments, late-type galaxies in low-local-density environments have lower HI detection fractions than their counterparts more than 5 Mpc from any filament, across all stellar mass bins, which the paper attributes to ram-pressure stripping and cosmic-web detachment acting on infalling galaxies.
Massive early-type galaxies in low-density filament sections show a higher HI detection fraction than in voids, suggesting that filamentary gas accretion or gas-rich mergers can replenish cold gas in galaxies that are usually HI-poor.
Local galaxy density and filament proximity are related but distinct environmental measures: controlling for one does not remove the other's effect on HI detection, so future environmental studies need to treat both scales.
The absence of a filament-proximity trend among high-local-density galaxies suggests that group-shielded galaxies are less susceptible to filament-driven gas removal, meaning the filament effect depends on how galaxies encounter the cosmic web.
An HI non-detection does not mean a galaxy has no HI; the detection-fraction variations indicate that the underlying HI mass distribution shifts with environment, motivating HI stacking experiments across cosmic-web environments.

Reading between the lines

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

If the paper's interpretation is right, HI spectral stacking of the non-detected galaxies near filaments should reveal a downward-shifted or broadened HI mass distribution compared with voids; the paper identifies this as a future direction but does not quantify the expected shift.
The same D_fil analysis applied to other 21-cm surveys at different sensitivities or redshifts would test whether the mass- and density-dependent reversal (late-type deficit versus early-type excess) is a universal cosmic-web effect or a sensitivity-dependent feature.
The stellar-mass–HI-mass relation may itself vary with filament proximity, which would matter for any application that infers gas content from stellar mass alone in large-scale structure studies.
If the enhanced HI fraction among massive early-types near filaments is genuine, HI-selected surveys that overlap with filamentary large-scale structure could be over-representing this rare population, affecting estimates of the HI mass function in such fields.

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Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

The headline: this is a serious observational paper that reports a new result—HI detection fractions around cosmic filaments vary with stellar mass and local density in opposite directions—but the statistics are thinner than the abstract claims, and one load-bearing check (redshift matching across D_fil bins) is asserted but never shown.

What's new: no one has measured HI detection fractions of DESI galaxies as a function of DisPerSE filament distance in COSMOS and XMM-LSS with these controls. The use of MIGHTEE-HI DR1 with untargeted source finding is a plus, and the paper is transparent about its sample construction. The jackknife filament catalogue and Monte Carlo p-values are reasonable. The finding that late-type galaxies in low-density regions have lower HI detection fractions close to filaments, while massive early-types show the opposite, is genuinely interesting and physically plausible.

Soft spots: the redshift matching issue is the most important. Section 3.1 says the samples being compared have similar redshift distributions, but no distributions, medians, or tests are shown. Given Fig. 4a shows a steep drop in detection fraction with redshift, unequal D_fil bins could produce the trends without any filament effect. The stress-test note is fair. Second, the abstract says 'across all stellar mass ranges' but Table 2 shows the intermediate-mass late-type cumulative p=0.369, which does not support that. Third, there are many unadjusted tests; p-values in the 0.03–0.04 range should be treated with caution. The D_node cut and density splits are defensible, but they were chosen post hoc. The filament catalogue built from the same DESI galaxies is standard practice, but it does mean D_fil is not fully independent of density.

Overall: the paper deserves a serious referee. The missing redshift checks and multiple-testing corrections are addressable. The central claim is plausible but not yet airtight. I'd send it to review, but ask for the redshift distributions and a multiple-testing adjustment before anything is final.

Referee Report

4 major / 6 minor

Summary. This paper uses 865 DESI spectroscopic galaxies in the COSMOS and XMM-LSS MIGHTEE-HI fields to measure the fraction detected in HI as a function of distance to the nearest DisPerSE cosmic filament, after binning by stellar mass, morphology, and local density. The authors report that late-type galaxies in low-local-density environments show reduced HI detection fractions close to filaments, while massive early-type galaxies in low-density filament regions show enhanced HI detection, and they interpret these trends as evidence for ram-pressure stripping, cosmic-web detachment, and gas accretion or mergers. The paper also confirms earlier findings that galaxies closer to filaments are more massive and more often early-type.

Significance. The study combines an untargeted HI survey with dense DESI spectroscopy and makes a serious attempt to separate filament effects from stellar mass, morphology, and local density, using jackknife filament realizations and Monte Carlo null tests. If the statistical concerns are resolved, the result would be an important step in connecting cold gas to the cosmic web at z<0.1. The main strengths are the independent HI source finding, the explicit control for stellar mass and morphology, and the treatment of local density as a separate environmental axis. The current manuscript, however, does not yet provide the redshift-distribution evidence needed to rule out an artefactual origin, and some headline claims exceed the significance shown in the tables.

major comments (4)

[Section 3.1, Figs 7-8] The paper states that 'we ensure that the samples being compared have similar redshift distributions,' but no redshift distributions, median redshifts, or statistical tests are presented for any D_fil bin or for the D_fil > 5 Mpc reference samples used in Figures 7 and 8. This is load-bearing because Fig. 4a shows the HI detection fraction drops steeply with redshift (attributed to Malmquist bias), and the survey contains strong LSS overdensities at z ~ 0.03, 0.045, 0.055, and 0.07. If galaxies at small D_fil are systematically at different redshifts than the reference, the reported low-density late-type suppression and early-type enhancement could be redshift artefacts. Please show the redshift histograms and median z per D_fil bin (and per mass/density subsample), report KS or similar tests, or apply redshift weighting/matching.
[Abstract; Section 3.4.2; Table 2] The abstract's claim that late-type galaxies in low-local-density environments show reduced HI detection 'across all stellar mass ranges' is not supported by Table 2. For the intermediate-mass bin (9 <= log M*/Msun < 10, low density), the cumulative p-value for D_fil < 3.6 Mpc is 0.369, and the text itself calls the inner bin tentative (p = 0.0791 with 8 galaxies). For the high-mass bin, there are no low-density late-type galaxies within D_fil < 1.2 Mpc, and the claimed deficit rests on two bins (cumulative p = 0.0403). Only the lowest-mass bin shows cumulative p = 0.0300. The wording of the abstract and summary should be revised to match these significance levels, or the analysis needs to be extended (e.g., HI stacking) to support the stronger claim.
[Tables 1-2; Section 3.4] The significance of the filament trends is evaluated with many correlated interval and cumulative tests (5 D_fil bins x 3 mass bins x density splits, for each morphology), and no multiple-testing correction is applied. For example, the p = 0.0119 for massive early-type low-density galaxies (bins with 6, 23, 16, 4, and 2 galaxies) would become p ~ 0.24 if a Bonferroni correction were applied over the ~20 interval tests in Table 2 alone. The authors should report the total number of tests and either apply an appropriate correction (e.g., false-discovery rate) or explicitly present the small-p results as tentative until confirmed with larger samples or stacking.
[Sections 2.3-2.4] The filament catalogue is built from the same DESI spectroscopic galaxy distribution that defines the optical sample, so D_fil is not an independent environmental variable; galaxies in overdensities are, by construction, more likely to be assigned small D_fil, and these same galaxies have lower HI detection fractions. The paper's central claim rests on the assumption that this coupling does not bias the comparison after controlling for local density. Because this is a standard methodology, I do not consider it disqualifying, but a robustness test would substantially strengthen the paper: e.g., build the filament catalogue from a version of the DESI sample that excludes the 865 science galaxies, or cross-check with an external void/filament catalogue, and repeat the key panels of Figures 7 and 8.

minor comments (6)

[Fig. 4a] The redshift axis covers 0.04-0.08 while the sample is defined over 0.02<z<0.09; please clarify the binning or the effective range used for the detection fraction.
[Section 2.2.2] The statement that the exact star-forming definition does not affect the results is not demonstrated; a short supplementary test would help.
[Throughout] The rendered 'Hi' and 'Hidetection' (missing space) should be harmonized to 'HI' and 'HI detection'.
[Section 3.4.3] For consistency with Fig. 8, please state the galaxy counts in the text when quoting the p=0.0119 result, since the innermost-bin count is only 6.
[References] The reference list entry for Maksymowicz-Maciata et al. (2026) lacks a volume/page; update if available.
[Section 4.2.1] The phrase 'the high HI detection fraction we observe among late-type galaxies in low-local density environments' is ambiguous because the main result is a decreased fraction near filaments; rephrase to 'the relatively high HI detection fraction of late-type galaxies in low-density environments away from filaments'.

Circularity Check

0 steps flagged · score 2.0 of 10

No significant circularity: the central filament-HI correlation is measured against independent MIGHTEE-HI data and is not derived from fitted inputs.

full rationale

The paper's central claim is an observational correlation between filament distance and HI detection fraction, built from two independent data products: D_fil is measured with DisPerSE from DESI spectroscopic galaxy positions (Section 2.4), while HI detection comes from untargeted source finding in the MIGHTEE-HI data cubes (Sections 2.1 and 5). No parameter is fitted to the HI data and then reported as a prediction; the analysis compares measured fractions in D_fil bins against a D_fil > 5 Mpc reference using binomial and Monte-Carlo significance tests (Section 3.4). The same DESI galaxy distribution is used both to construct the filament skeleton and to define the optical sample, which couples D_fil to galaxy density (Fig. 3), but this is a standard tracer choice and not a definitional reduction: D_fil is not defined in terms of either local density or HI content. Self-citations such as 'Following Tudorache et al. (2025), we construct 100 input galaxy catalogues jack-knifed from the full sample' and the use of the Maksymowicz-Maciata et al. (2026) catalogue are methodological and not load-bearing; the filament identification itself rests on the public DisPerSE algorithm. The one assertion needing scrutiny is Section 3.1's statement that 'we ensure that the samples being compared have similar redshift distributions,' which is not demonstrated for the D_fil bins or the reference samples; combined with the steep redshift dependence in Fig. 4(a), this is a potential confound that should be checked, but it is an internal-validity issue, not circularity. The paper does not reduce its conclusions to its inputs by construction, so no circular step is identified; the score of 2 reflects minor self-citations and a mild tracer coupling without any load-bearing circular reduction.

Assumptions & free parameters 8 free parameters · 7 assumptions · 0 invented entities

No new physical entities are postulated; interpretations invoke known mechanisms (ram pressure stripping, cosmic web detachment, mergers) from prior literature. The free parameters are analysis choices that affect the reported trends and p-values.

free parameters (8)

HI mass limit log M_HI/Msun > 8.7 = 8.7
Applied to define a consistent HI sample; affects which galaxies count as detections and the completeness.
Stellar mass limit log M*/Msun > 8.5 = 8.5
Applied for stellar-mass completeness of the optical sample; changes sample composition.
Local density split for late-type galaxies = log Sigma5 = 0 Mpc^-2
Divides low- and high-density samples; the threshold is chosen by hand and affects the inferred D_fil trend.
Local density split for early-type galaxies = log Sigma5 = 0.5 Mpc^-2
Higher threshold used because early-type galaxies occupy denser environments.
Node exclusion distance D_node = 2 Mpc
Galaxies within 2 Mpc of nodes are excluded; authors tested 1, 3, and 5 Mpc and report results unchanged.
Filament persistence threshold = 3.5 sigma
DisPerSE parameter motivated by Sousbie et al. (2011); determines which filament structures are kept.
D_fil bin width = 1.2 Mpc
Radial binning for filament profiles; affects p-values and apparent trends.
Reference sample threshold = 5 Mpc
Galaxies with D_fil > 5 Mpc define the reference sample; changes the baseline fraction.

assumptions (7)

domain assumption DisPerSE with persistence threshold above 3 sigma removes spurious filaments and yields a faithful filament network.
Invoked in Section 2.4; if false, D_fil is not a reliable environmental measure.
domain assumption The DESI spectroscopic galaxy sample used for filament finding is a homogeneous, unbiased tracer of the large-scale structure in the 30x30 degree fields.
Section 2.4 prioritises homogeneity; phase-dependent sampling could bias the filament network.
domain assumption Unmatched HI sources, especially the 40% in XMM-LSS, do not bias the HI detection fraction analysis.
Section 2.3 assumes no significant population bias from incomplete matching.
domain assumption The HI mass limit gives a redshift-independent completeness (average 95.5% in COSMOS), so detection fraction differences reflect physical gas content rather than sensitivity.
Section 3 states this using Maksymowicz-Maciata et al. (2026); if completeness varies with environment, trends could be instrumental.
domain assumption Compared samples have similar redshift distributions.
Section 3.1 says this is ensured, but no table or figure demonstrates it; given strong Malmquist bias in Fig. 4a, this is load-bearing.
standard math Standard Planck 2016 Lambda-CDM cosmology.
Used for distances and cosmology; not controversial.
domain assumption The 5th-nearest-neighbour projected density with photo-z resampling traces local environment without residual bias.
Section 2.5; if photo-z errors correlate with filament proximity, density control may be incomplete.

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Cite this review

Pith. "Pith review of MIGHTEE-HI: Environmental effects of cosmic filaments on extragalactic HI detections in the COSMOS and XMM-LSS fields." pith.science (2026). https://pith.science/paper/EMKKESMB

@misc{pith2026260804656,
  author       = {Pith},
  title        = {Pith review of: MIGHTEE-HI: Environmental effects of cosmic filaments on extragalactic HI detections in the COSMOS and XMM-LSS fields},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/EMKKESMB}},
  note         = {Machine review of arXiv:2608.04656}
}

abstract

Cosmic filaments have been recognised as influencing galaxy evolution, but their connection to galactic cold gas reservoirs is elusive, particularly at low redshifts. We investigate the influence of filaments on neutral hydrogen (HI) detections in galaxies at $0.02<z<0.09$, using the MeerKAT International GHz Tiered Extragalactic Exploration (MIGHTEE) survey in the COSMOS and XMM-LSS fields. We measure the fraction of optical galaxies from the Dark Energy Spectroscopic Instrument (DESI) Survey detected in HI emission as a function of stellar mass, morphology, local density, and the distance to the nearest filament. We find that galaxies closer to filaments have higher stellar masses, higher local densities, and a larger early-type fraction, all of which affect the HI detection. After controlling for these dependencies, filaments have measurable effects on HI detection. Late-type galaxies in low-local density environments show reduced HI detection fractions close to filaments across all stellar mass ranges, suggesting potential gas depletion through ram pressure stripping and cosmic web detachment. Massive early-type galaxies show an enhanced HI detection fraction in filaments compared to the voids, suggesting possible gas replenishment through filamentary accretion or gas-rich mergers. Our results suggest that cosmic filaments influence galactic HI gas reservoirs through various competing processes, whose relative importance varies with stellar mass and local density.

Figures

Figures reproduced from arXiv: 2608.04656 by the authors.

**Figure 1.** Top panel: Hi mass as a function of redshift. Brown dots are galaxies satisfying the Hi mass limit adopted in this study (log 𝑀HI/M⊙ > 8.7; horizontal dashed line). The solid line shows their median Hi mass in redshift bins of Δ𝑧 = 0.005. The grey dots are galaxies below the mass limit. Middle panel: Same format as the upper panel, showing the stellar mass of the optical sample as a function of redshift and the stel… view at source ↗

**Figure 2.** Distribution of cosmic filaments identified with DisPerSE in the COSMOS (left) and XMM-LSS (right) fields. The blue lines show filaments within ±1 ◦ of the declination centre of each MIGHTEE-Hi field. The low opacity of the lines is set to highlight regions where filaments from the 100 jackknife realisations overlap. The grey lines show the remaining filaments in the 30◦ × 30◦ fields. The vertical dashed lines are t… view at source ↗

**Figure 3.** The local density (log Σ5) and the distance to the nearest cosmic filament (𝐷fil) of the late-type (blue dot) and early-type (red cross) galaxies. The solid and dashed lines show the median log Σ5 of late- and early-type galaxies as a function of 𝐷fil. The black dots are galaxies within 𝐷node ⩽ 2 Mpc. 2023; hereafter photo-z catalogues). As the photometric redshift catalogues include both stars and galaxies, we ado… view at source ↗

Figures from the paper (4 more)

**Figure 4.** Figure 4: Hi detection fraction (red solid line for all optical galaxies; red dashed line for star-forming galaxies only) and star-forming galaxy fraction (blue dotted line) of optical galaxies as a function of redshift, stellar mass, Sérsic index, and local density (from top to…

**Figure 5.** Figure 5: Hi detection fraction of late-type galaxies as a function of local density. Each colour represents different stellar mass bin: 8.5 < log 𝑀∗/M⊙ < 9 (blue solid line), 9 ⩽ log 𝑀∗/M⊙ < 10 (green dashed line), and log 𝑀∗/M⊙ ⩾ 10 (red dotted line). The error bars show the …

**Figure 7.** Figure 7: Top panels: Hi detection fraction as a function of 𝐷fil, for late-type galaxies in different local densities (log Σ5/Mpc−2 < 0). The error bars show the 68% Jeffrey’s credible interval. The three columns correspond to three stellar mass bins: 8.5 < log 𝑀∗/M⊙ < 9 (left)…

**Figure 8.** Figure 8: The same format as [PITH_FULL_IMAGE:figures/full_fig_p010_8.png]

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