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REVIEW 5 major objections 5 minor 129 references

This paper claims that the average neutral hydrogen fraction of cluster galaxies stays below the field level out to five times the virial radius, implying gas is stripped from galaxies before they enter the cluster core.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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Stacked FAST spectra show cluster galaxies have less neutral hydrogen than field galaxies out to 5R200, including blue star-forming members.

T0 review reviewed 2026-08-01 challenge →

load-bearing objection Solid internal radial trend; the beyond-virial claim needs a matched field control before it carries. the 5 major comments →

arxiv 2607.25800 v1 pith:YT2WSIK5 submitted 2026-07-28 astro-ph.GA

HI Depletion Begins Well Beyond the Virial Radius: A FAST Stacking Study of 36 Galaxy Clusters to 5R200

Cheng Cheng , Chuan-Peng Zhang , Edo Ibar , Rory Smith , Weiwei Xu , Hyowon Kim , Jia-Sheng Huang , Wei Zhang
show 5 more authors
Pei Zuo Hugo M\'endez-Hern\'andez Juan Molina Ming Zhu Qian Yu
This is my paper
classification astro-ph.GA
keywords HI 21-cmgalaxy clustersenvironmental quenchingram-pressure strippingpre-processingspectral stackingFASTDESI
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.

The reading

The paper stacks 21-cm neutral hydrogen spectra of galaxies around 36 massive clusters to measure the average HI content as a function of cluster-centric distance. It finds that both the average HI mass and the HI-to-stellar-mass ratio decline inward, and that the HI fraction at 5×R200 remains about 0.3–1 dex below field galaxies of the same color and stellar mass. The authors interpret this as statistical evidence that environmental gas removal begins in the cluster outskirts, in groups and filaments, before galaxies reach the dense core. If true, this moves the onset of quenching far earlier than the virial radius.

Core claim

Using spectral stacking of FASHI survey data with DESI spectroscopic members, the authors show that the average HI-to-stellar mass ratio of cluster members is suppressed relative to field galaxies at all projected radii out to 5R200, with a decline of roughly 0.5 dex from outskirts to center. The deficit persists when galaxies are split by g−r color, so even optically blue, star-forming cluster members have lower gas fractions than field galaxies of the same color. This is presented as direct statistical evidence that cold gas is stripped from galaxies in the cluster outskirts, likely in infalling groups and filaments, prior to full optical transformation.

What carries the argument

The analysis rests on spectral stacking of HI 21-cm emission from the FAST all-sky survey, which recovers average flux from hundreds of galaxies per bin that are individually undetected. Membership is assigned using a projected phase-space boundary from an NFW escape-velocity profile scaled by flos = 0.7 and a velocity-dispersion–mass relation, and a blending correction combines galaxies within the 3-arcmin beam to avoid double-counting.

Load-bearing premise

Membership at 2–5R200 is defined by an approximate escape-velocity boundary; if interloper rejection or spectroscopic incompleteness correlates with HI content, the apparent deficit at large radius could be a selection artifact rather than genuine stripping.

What would settle it

A stacking analysis that splits the 4–5R200 sample into galaxies well inside versus near the assumed escape boundary, or uses high-resolution interferometric data to confirm membership and resolve blends, would settle the claim: if the field-normalized HI deficit vanishes when interlopers are removed, the pre-processing conclusion fails.

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

If this is right

  • The finding implies that HI depletion is not confined to cluster cores but begins in the large-scale feeding structures around clusters.
  • The observed deficit among blue, star-forming cluster members indicates that gas removal precedes optical color transformation, constraining the timescale of quenching.
  • The transition radius near 2R200 aligns with the extent of hot X-ray gas, suggesting a common physical boundary where infalling galaxies first encounter stripping conditions.
  • The total HI content in clusters and their outskirts roughly matches TNG simulations, supporting current models of gas accretion and feedback in massive halos.
  • The lack of a strong relaxed-versus-disturbed difference suggests that global dynamical state plays a minor role in the average HI content of member galaxies.

Where Pith is reading between the lines

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

  • If the deficit at 5R200 is real, high-resolution HI imaging of galaxies in that region should reveal truncated disks, asymmetric extraplanar gas, or tails pointing away from the cluster center even well outside the virial radius.
  • The mass-dependent onset of depletion (dwarf galaxies decline earlier than massive ones) could be tested by correcting for blending with interferometric observations; if the trend survives, it points to shallow-potential galaxies being stripped by gentler mechanisms in the outskirts.
  • The paper's own discussion implies the field-galaxy baseline itself is environment-dependent, so the 'deficit' could partially reflect that the comparison sample occupies an average cosmic density higher than true voids; quantifying this would sharpen the pre-processing claim.
  • A joint analysis of HI stacking with filament identification (e.g., splitting members by proximity to filament spines) would directly test whether the outskirts deficit is driven by galaxies in filaments rather than those falling in from lower-density regions.
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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

5 major / 5 minor

Summary. The paper stacks FAST/FASHI 21-cm spectra at the positions of DESI/SGA spectroscopic member galaxies of 36 AXES X-ray clusters at z<0.07, measuring average M_HI and M_HI/M* in three stellar-mass bins and six projected radial bins out to 5R200. The authors report a monotonic decline of M_HI and M_HI/M* toward cluster centers, interpret the turnover near ~2R200 as the splashback/shock radius, and claim that M_HI/M* remains below the field value even at 4.5–5.5R200, which they attribute to pre-processing in filaments and infalling groups. They further report that the HI deficiency persists at fixed g−r color, that relaxed and disturbed clusters show no significant difference, and that integrated HI masses are broadly consistent with TNG simulations. The internal radial trend is based on a large, uniformly selected sample with conservative resampling-based errors; the headline claim about depletion at 5R200, however, rests on comparisons with external or HI-selected field baselines that are not matched to the cluster sample.

Significance. If firmly established, the claim that cold-gas depletion begins well beyond the virial radius would provide a direct gas-phase counterpart to earlier star-formation suppression observed at 2–5R200 and would strengthen the pre-processing scenario in cluster outskirts. The paper's strengths include the large stacking sample (~170 to >1000 spectra per bin), the use of conservative resampling uncertainties, the public HISS stacking code, and unusually candid discussion of beam-blending, incompleteness, and the approximate nature of the membership boundary. However, the central claim is not yet supported at the quoted significance: the 5R200 offset is described in the text as 1σ, and the field baselines used in Figs. 5 and 7 are not selected or processed in the same way as the cluster sample. These issues are load-bearing and need to be addressed before the paper's main conclusion can be accepted.

major comments (5)
  1. [§4.1, Fig. 5] The text states that at large cluster-centric distances the average M_HI/M* 'remains 1σ lower' than the Guo et al. (2021) field relation. A 1σ offset is not a statistically significant detection, yet the abstract and §6 conclude that M_HI/M* 'remain lower than field galaxies even at the 5R200' and that this 'provides direct, statistical evidence.' Please report the actual offset, its 1σ uncertainty, and the significance level for the 4.5–5.5R200 bin. If the offset is indeed only 1σ, the headline claim should be softened accordingly.
  2. [§4.1, Fig. 5] The field reference from H. Guo et al. (2021) is an ALFALFA stacking analysis with a different survey footprint, depth, angular resolution, target selection, and spectral extraction pipeline, while the cluster sample is mass-selected from DESI and includes non-detections. The apparent deficit at 5R200 is therefore not a matched comparison. A matched field control drawn from the same DESI/FASHI parent sample, processed through the same extraction, stacking, and blending pipeline, is needed before claiming depletion beyond the virial radius. The internal radial decline would not be erased by such a control, but the normalization offset could change.
  3. [§4.2, Fig. 7] The color-resolved comparison uses FASHI-detected field galaxies, which are by construction HI-selected and therefore gas-rich, while the cluster members are mass-selected and include non-detections. This selection asymmetry alone can produce an apparent deficiency. The statement that this bias is 'modest in the g−r plane' is not quantified, and no matching in stellar mass or redshift is shown. The 0.3–1 dex offsets in Fig. 7 cannot be interpreted as environmental HI deficiency until a mass- and color-matched field sample including non-detections is stacked with the same pipeline.
  4. [§3.2] The blending correction rescales cluster M_HI by a factor N_stacking/N_total, typically about 0.7 (≈0.15 dex), and up to 0.2 dex for the low-mass bin. The Guo et al. (2021) field baseline has not been subjected to this correction. Because the field reference is not processed through the same blending treatment, a systematic offset of order 0.15–0.2 dex is introduced into the cluster/field comparison. This is comparable to the quoted 1σ offset at 5R200 and must be propagated or removed by applying an identical correction to a matched field sample.
  5. [§2.3, Eq. (2)] The phase-space membership boundary uses an NFW escape-velocity profile with f_los=0.7 and the Evrard et al. (2008) velocity-dispersion scaling. The paper itself cautions that at R>2R200 the uncertainties grow substantially due to breakdown of spherical symmetry, interlopers, and the assumed mass profile. Since the headline claim concerns the 4.5–5.5R200 bin, the sensitivity of the stacked M_HI to reasonable changes in f_los (e.g., 0.6–0.8), to the concentration–mass relation, and to interloper rejection should be quantified. Without such robustness tests, it is unclear whether the outermost bin mean reflects true members or a mixture whose selection could be HI-correlated.
minor comments (5)
  1. [Introduction/§2.1.3] FASHI coverage is quoted as ~4000 deg² in the introduction and ~19,500 deg² in §2.1.3. Please clarify that the smaller number refers to DR1 and the larger to current/DR2 coverage.
  2. [Fig. 5 caption] The caption says 'There are systematically less targets in the 5R/R200 bins'; change 'less' to 'fewer' and clarify that the outermost bin corresponds to 4.5–5.5R200.
  3. [§5.4] The section title appears as '–Halo Relation Across a Broad Halo Mass Range'; the omitted 'M_HI' should be restored.
  4. [§3.2] The notation 'M_avg code HI' and 'M_avg corr HI' is hard to parse; define the superscripts/subscripts more clearly and use a consistent typographic convention.
  5. [Table 1] The Stage column contains '—' for five clusters; the text explains the reason, but adding a footnote to the table would improve readability.

Circularity Check

0 steps flagged

No circular derivation chain: the stacked HI measurements are not fitted to the field baselines, and the self-citations are data/method sources rather than load-bearing assumptions.

full rationale

The paper's central result is a spectral-stacking measurement of FAST/FASHI spectra at DESI/SGA galaxy positions, divided into mass/radius/color bins. The claim that M_HI/M* declines inward and remains below field values at ~5R200 is a comparison between these new stacked averages and external field references (H. Guo et al. 2021; FASHI field sample of C. Cheng et al. 2025a). Nothing in the stacking pipeline forces the cluster averages to lie below these baselines: the cluster fluxes are free to be higher or lower, and the quoted offset is only ~1 sigma. The phase-space membership (Eq. 2) uses f_los=0.7 from Diaferio (1999) and the Evrard et al. (2008) sigma-M scaling, adopted from the literature rather than tuned to reproduce the HI result. The blending correction (Sec. 3.2) is an empirical factor N_stacking/N_total applied to cluster averages; although it is not applied to the field baseline and could bias the comparison, it is not a fitted parameter that encodes the conclusion. The paper itself flags the main limitations: the membership boundary is approximate beyond ~2R200 (Sec. 2.3), beam blending is the primary uncertainty (Secs. 3.2, 5.1), and the dwarf-bin trends may be a systematic effect of the blending correction (Sec. 5.6). Self-citations (FASHI data papers, Kim et al. 2026 morphological classifier) are normal attributions to data and methods; they are not used to forbid alternatives or to define the target quantity in terms of the result. No equation in the paper reduces the claimed environmental signal to an input parameter by construction.

Axiom & Free-Parameter Ledger

3 free parameters · 7 axioms · 0 invented entities

The analysis introduces no new physical entities; it uses existing surveys, standard NFW modeling, and literature scaling relations. The main load-bearing choices are the f_los membership projection, the FAST beam blending thresholds, and the extraction aperture, all of which are acknowledged as sources of systematic uncertainty.

free parameters (3)
  • f_los projection factor = 0.7
    Adopted from Diaferio (1999) simulation range 0.6-0.8 to convert 3D escape velocity to line-of-sight. It sets the membership boundary in Eq. 2 and therefore defines the sample at 2-5R200.
  • Blend combination radius and velocity offset = 3 arcmin, Delta-V < 300 km/s
    Galaxies within these thresholds are merged into one stacked target, removing ~30% of galaxies and adding a 0.15-0.2 dex correction to stacked M_HI. The threshold choice directly affects the dwarf-bin trends (Section 3.2).
  • Extraction aperture = 6 arcmin diameter (approx 140-400 kpc depending on z)
    Fixed angular aperture used to extract HI spectra. The aperture-size systematic is quoted as up to ~0.3 dex from DePalma et al. in Section 5.1, so the choice affects absolute M_HI/M* values.
axioms (7)
  • domain assumption Cluster dark matter halos follow an NFW potential with the Duffy et al. (2008) concentration-mass-redshift relation (Eq. 1).
    Used to define the escape-velocity profile for membership selection; the paper itself states this is only approximate at large radii.
  • domain assumption The projected escape-velocity envelope is f_los=0.7 times the 3D escape velocity, independent of radius and anisotropy.
    Adopted from the literature and critical for selecting members at 2-5R200, where interlopers and spherical-symmetry breakdown are acknowledged problems.
  • domain assumption Velocity dispersion scales with M200 via the Evrard et al. (2008) relation, Eq. 3.
    M200 from AXES and this scaling set the vertical axis of the phase-space trumpet; scatter in the scaling propagates into membership.
  • domain assumption Missing spectroscopy is not strongly correlated with HI content in a way that differs across radial bins.
    Stated in Section 2.1.2. If false, the radial trend could be biased; the authors note incompleteness is worst in dense cores for quenched dwarfs, which would bias stacked HI upward at small radii.
  • domain assumption The 6 arcmin aperture contains most HI of a cluster galaxy and misses only a small diffuse component.
    Stated in Section 3.3 and Section 5.1; DePalma et al. (2025) indicates aperture-size systematics up to ~0.3 dex, so this is not exact.
  • domain assumption The Guo et al. (2021) ALFALFA stacking relation is a valid field baseline for M_HI/M* at fixed stellar mass.
    This is the central comparison in Section 4.1; it uses a different telescope, survey, and selection than the cluster stacking, with no matched same-pipeline control.
  • domain assumption FASHI-detected field galaxies are representative of field galaxies by g-r color, with only a modest gas-rich bias.
    Used for the color-resolved comparison in Section 4.2; the bias is discussed qualitatively but not corrected quantitatively.

reviewed 2026-08-01 · how reviews work

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Cite this review

Pith. "Pith review of HI Depletion Begins Well Beyond the Virial Radius: A FAST Stacking Study of 36 Galaxy Clusters to 5R200." pith.science (2026). https://pith.science/paper/YT2WSIK5

@misc{pith2026260725800,
  author       = {Pith},
  title        = {Pith review of: HI Depletion Begins Well Beyond the Virial Radius: A FAST Stacking Study of 36 Galaxy Clusters to 5R200},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/YT2WSIK5}},
  note         = {Machine review of arXiv:2607.25800}
}
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abstract

We present a stacking study of the neutral atomic hydrogen (HI) content in and around 36 local galaxy clusters at $z<0.07$, using a combination of the FAST all sky HI survey (FASHI) and the extensive spectroscopic catalog mainly from the Dark Energy Spectroscopic Instrument (DESI). We employ spectral stacking techniques to probe the average HI mass and HI-to-stellar mass ratio ($M_{\rm HI}/M_*$) for member galaxies down to stellar masses of $M_*\sim 10^9M_\odot$, spanning a projected cluster-centric distance to $5R_{200}$. Our analysis reveals a pronounced environmental effect: both $M_{\rm HI}$ and $M_{\rm HI}/M_*$ decrease steadily towards the cluster center, dropping by $\sim 0.5$ dex on average from the outskirts to the core. Crucially, we find that $M_{\rm HI}/M_*$ of galaxies remain lower than the field galaxies even at the $5R_{200}$. This provides direct, statistical evidence for substantial gas stripping and pre-processing in the cluster outskirts, likely occurring in infalling groups and large-scale filaments. By further splitting the sample by $g-r$ color, we show that the HI deficiency persists at fixed galaxy color: even the bluest cluster members exhibit $\sim 0.5$~dex lower $M_{\rm HI}/M_*$ than field galaxies of similar color, reflecting environmental effects on the cold gas reservoir prior to full optical transformation. The total HI mass within clusters and their outskirts agrees broadly with predictions from cosmological simulation. Our results underscore the critical role of the extended cluster environment in quenching galaxies by depleting their cold gas reservoirs well before they enter the dense cluster core.

Figures

Figures reproduced from arXiv: 2607.25800 by Cheng cheng, Chuan-Peng Zhang, Edo Ibar, Hugo M\'endez-Hern\'andez, Hyowon Kim, Jia-Sheng Huang, Juan Molina, Ming Zhu, Pei Zuo, Qian Yu, Rory Smith, Weiwei Xu, Wei Zhang.

Figure 1
Figure 1. Figure 1: Lower panel: The velocity–distance distribution for all sample clusters. The green lines mark the boundaries defined by Equation 2. The blue, red and green dots are cluster members in low mass bin (8.5 < log(M∗/M⊙) < 9.5), medium mass bin (9.5 < log(M∗/M⊙) < 10.5) and high mass bin (10.5 < log(M∗/M⊙)). The black dots are the targets close to the clusters, yet not bounded by the cluster. Upper panel: Galaxy… view at source ↗
Figure 2
Figure 2. Figure 2: Left: Redshift vs M∗ of the member galaxies we selected. The stellar mass lower to 109M⊙ is not complete to the redshift 0.06. The dashed purple line shows the stellar mass for a target with r = 20 AB mag and g − r = 0.5 at each redshift, which is roughly the detection limit of the DESI spectroscopic sample. Right: Histogram of the stellar mass at different R/R200. The stellar mass distribution for galaxie… view at source ↗
Figure 3
Figure 3. Figure 3: The ratio of the number of targets for stacking and all galaxy numbers. The black line is the total number ratio for all member galaxies, and the blue, green and red lines are the low, medium and high mass bin galaxy members. We denote the number of stacking targets and number of total galaxies in each mass and radius bin near the ratio. is different at M∗ ∼ 3 × 1010M⊙, above which the old stellar populati… view at source ↗
Figure 4
Figure 4. Figure 4: Stacking H i spectra for the 18 bins. The top, middle and bottom panels are the stacking results for low, medium and high mass bins, respectively. The R/R200 for each column is denoted on top of the panels. The stacked H i spectra do not show double horn profile, but single-peaked or top-flatted. So we fit the H i flux by gaussian function, and obtain the H i mass by the gaussian fitting. The shaded region… view at source ↗
Figure 5
Figure 5. Figure 5: Left: Averaged H i mass at different radius for the low mass bin (blue), medium mass bin (green) and high mass bin (red).The shaded regions represent the uncertainties of the stacking results. We use shaded regions with hatching for the low-mass bins to emphasize the stellar-mass incompleteness ( [PITH_FULL_IMAGE:figures/full_fig_p012_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Left panel: Averaged H i mass MHI/M∗ at different radius (color dots). Results from ALFALFA stacking re￾sults (open triangles H. Guo et al. 2021), xGASS project (open circles B. Catinella et al. 2018) and HI-selected sample from MIGHTEE-HI project (H. Pan et al. 2023) are shown for comparisons. Our mass-selected sample (open colored circles) shows the lowest MHI/M∗ values among the samples. Previous studie… view at source ↗
Figure 7
Figure 7. Figure 7: Stacked MHI/M∗ as a function of g − r color. Small black dots show individual FASHI-detected field galaxies. Colored symbols with error bars denote the stacked ⟨MHI/M∗⟩ measurements for cluster member galaxies in different projected cluster-centric distance bins, as indicated in the legend. Different symbols represent the three stellar mass bins: triangles for 8.5 < log M∗/M⊙ < 9.5, squares for 9.5 < log M… view at source ↗
Figure 8
Figure 8. Figure 8: Same as [PITH_FULL_IMAGE:figures/full_fig_p015_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Same as [PITH_FULL_IMAGE:figures/full_fig_p016_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Average H i mass (top panel) and average HI– to-stellar mass ratio (bottom panel) in different radial and mass bins for galaxies in relaxed clusters (open squares) and disturbed clusters (open diamonds), compared with the full cluster sample (open circles). For clarity, data points at the same radial bin are horizontally offset by 0.1 dex to avoid overlapping error bars; the offset has no physical meaning… view at source ↗
Figure 11
Figure 11. Figure 11: H i total mass in each clusters within 2R200 (red squares) or 2R200 < R < 5R200 (blue solid dots), in comparison with the simulation results from TNG Clusters (green diamonds D. Nelson et al. 2024) and TNG300 (coral boxes A. Pillepich et al. 2018; D. Nelson et al. 2018; J. P. Naiman et al. 2018; F. Marinacci et al. 2018; V. Springel et al. 2018). H i abundances from SDSS data from A. Obuljen et al. (2019)… view at source ↗
Figure 12
Figure 12. Figure 12: H i mass as a function of halo mass over a wide mass range. The integrated H i mass within R < 2R200 (red squares) and 2R200 < R < 5R200 (blue solid circles) for individual clusters is shown. The MHI-Mhalo relations for group galaxies from A. Obuljen et al. (2019) and H. Guo et al. (2017) are shown as black open circles and open squares, respectively. The HI-selected dwarf galaxies (MHI < 108 M⊙) are show… view at source ↗

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This paper was first reviewed by deepseek-v4-flash on August 1, 2026.