Anisotropic quenching beyond $z=1$ and its implications for preprocessing around high-redshift galaxy clusters

Kazuhiro Shimasaku; Kei Ito; Makoto Ando; Suin Matsui; Takumi S. Tanaka

REVIEW 3 major objections 2 minor 300 references

Anisotropic quenching beyond $z=1$ and its implications for preprocessing around high-redshift galaxy clusters

T0 review · 3 major / 2 minor · reviewed 2026-06-26 · grok-4.3

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Pith's one-line read Preprocessing before cluster entry explains the anisotropic quenching seen in galaxy clusters at redshifts 0.9 to 1.4.

desk verdict Modest 2-sigma anisotropic quenching signal at z>1, but the preprocessing dominance claim comes from a semi-analytic model whose parameters lack independent anchors. read the letter →

arxiv 2606.23790 v1 pith:QPN5G2BM submitted 2026-06-22 astro-ph.GA

Makoto Ando , Kazuhiro Shimasaku , Kei Ito , Takumi S. Tanaka , Suin Matsui This is my paper · ORCID

classification astro-ph.GA

keywords anisotropicquenchinggalaxyclusterspreprocessingsatellitegalaxieshigh-redshiftmechanismscosmologicalsimulationsenvironmentaleffects

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

The paper measures a modest preference for quenched satellites along the major axis of the central galaxy in 12 clusters at 0.9 < z < 1.4. Simulation accretion histories show that most satellites arrived within the past 2 Gyr and lose their orientation memory on a comparable timescale. A semi-analytic model that folds these histories into a delay-then-rapid quenching prescription finds that galaxies quenched outside the cluster dominate the signal and produce a 20 percent higher quenched fraction along the major axis than the minor axis, matching the data.

What carries the argument

A semi-analytic model that integrates simulation-derived satellite accretion histories with a delay-then-rapid quenching framework, explicitly parameterizing the separate contributions from intrahalo quenching and preprocessing.

What would settle it

Measuring the major-minus-minor axis difference in quenched fraction for only those satellites accreted more than 2 Gyr ago and finding that the difference remains as large as for the full population would falsify the claim that recent accretion and preprocessing drive the anisotropy.

Watch

Extended reading notes

Core claim

In 12 spectroscopically confirmed galaxy clusters at 0.9 < z < 1.4, the quiescent satellite fraction is higher along the major axis of the central galaxy. Cosmological simulations indicate that most satellites in z = 1.25 clusters have been accreted within the last 2 Gyr and that their orientations randomize on a similar timescale. A semi-analytic model combining these accretion histories with a delay-then-rapid quenching framework shows that preprocessing is the main driver of quenching, with the preprocessing contribution being approximately 20 percent higher along the major axis than the minor axis, thereby reproducing the observed anisotropic quenching.

Load-bearing premise

The semi-analytic model correctly separates quenching that occurs inside the cluster from quenching that occurs beforehand in the surrounding large-scale structure.

Editorial extensions

If this is right

Preprocessing contributes more to satellite quenching than processes inside the cluster for these high-redshift systems.
The anisotropy is carried exclusively by satellites accreted within the last ~2 Gyr whose orientations have not yet randomized.
The ~20 percent excess quenched fraction along the major axis arises because preprocessing is stronger for galaxies that fall in along the filamentary directions aligned with the central galaxy.
Anisotropic quenching can therefore serve as a clock for the timing of environmental effects outside clusters.

Reading between the lines

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

If preprocessing already dominates at z > 1, then the environmental transformation of galaxies begins in filaments and groups well before cluster assembly.
The short ~2 Gyr randomization timescale implies that orientation memory from large-scale structure is transient, so larger samples at slightly lower redshift could map how the anisotropy fades as satellites spend more time inside clusters.
The same modeling approach could be applied to lower-redshift clusters to test whether the relative importance of preprocessing declines as clusters grow and intrahalo processes become more efficient.

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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.

Desk Editor's Note

read the letter

The main takeaway is a first reported detection of anisotropic quenching at 0.9

They examine 12 spectroscopically confirmed clusters, compute the quiescent satellite fraction versus angle from the central galaxy major axis, and find a preference along the major axis at roughly 2 sigma. The simulation shows that at z=1.25 most satellites are recent infallers within 2 Gyr and that orientations randomize on that timescale, limiting the anisotropy to recently accreted galaxies.

The semi-analytic piece combines those histories with a delay-then-rapid quenching framework. It splits quenching into intrahalo and preprocessing channels, then reports that preprocessing produces a 20% higher quenched fraction along the major axis and reproduces the observed anisotropy.

The simulation link between accretion timing and preserved orientation is a clear step forward and stands on its own. The observational extension to z>1 is also useful for people tracking when environmental effects set in.

The soft spot is the model. Both channels are parameterized, and the relative efficiencies are adjusted to match the 20% difference. No external constraint such as radial quenched profiles, stellar-mass trends, or field comparisons at the same epoch is shown to fix those parameters. The low significance of the data makes the result more sensitive to those choices.

This is for researchers modeling environmental quenching in high-redshift clusters. The accretion analysis could be cited for timing arguments even if the full interpretation is revised. It deserves peer review because the high-z detection is new and the paper is internally consistent; referees can check whether the model parameters survive additional tests.

Referee Report

3 major / 2 minor

Summary. The manuscript reports a ~2σ detection of anisotropic quenching among satellite galaxies in 12 spectroscopically confirmed clusters at 0.9<z<1.4, with higher quiescent fractions along the major axis of the central galaxy. Using cosmological simulations at z=1.25, the authors find that most satellites are recently accreted (≲2 Gyr) and that orbital orientations randomize on a comparable timescale. They then apply a semi-analytic model based on the delay-then-rapid quenching framework that separately parameterizes intrahalo quenching and preprocessing; the model attributes the observed anisotropy to preprocessing, which produces a ~20% higher quenched fraction along the major axis than the minor axis.

Significance. If the separation of quenching channels can be shown to be robust rather than tuned, the result would strengthen the case that preprocessing in large-scale structure dominates anisotropic quenching at z>1 and would have implications for how filamentary accretion shapes satellite populations. The combination of high-redshift observations, simulation-derived accretion histories, and explicit modeling of two quenching channels is a constructive approach; however, the modest statistical significance and lack of independent model validation limit the strength of the conclusions at present.

major comments (3)

[semi-analytic modeling section] The semi-analytic model (described after the simulation analysis) explicitly introduces free parameters for both intrahalo quenching and a preprocessing efficiency contrast between major and minor axes. No section demonstrates that these parameters are constrained by any observable other than the anisotropy signal itself (e.g., no radial quenched-fraction profiles, stellar-mass trends, or field-galaxy comparisons at the same epoch are shown to anchor the relative efficiencies). Consequently the reported ~20% major-axis excess may be reproduced by construction once the preprocessing contrast is allowed to vary.
[observational results] The observational detection is stated to be only ~2σ. Because the central claim that preprocessing dominates and reproduces the anisotropy rests on this marginal signal, the quantitative conclusion that preprocessing accounts for the full observed difference requires a clearer assessment of how the result changes when the significance threshold or sample definition is varied.
[simulation accretion history analysis] The simulation analysis concludes that orientation angles randomize in ~2 Gyr and that only recently accreted galaxies contribute to the anisotropy. It is not shown whether this timescale or the accretion history at z=1.25 remains consistent when the same analysis is repeated on the observed cluster sample or on lower-redshift comparison simulations.

minor comments (2)

[observational methods] The abstract and main text should state the exact number of satellites used for the orientation-angle measurement and the precise definition of the major-axis angle binning.
[figures] Figure captions for the quenched-fraction vs. angle plots should include the Poisson or bootstrap uncertainties on each bin so that the ~2σ claim can be directly verified from the figure.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We are grateful to the referee for their detailed and constructive feedback on our manuscript. We have carefully considered each major comment and provide point-by-point responses below. Where appropriate, we outline revisions that will be incorporated into the next version of the paper to address the concerns raised.

read point-by-point responses

Referee: The semi-analytic model (described after the simulation analysis) explicitly introduces free parameters for both intrahalo quenching and a preprocessing efficiency contrast between major and minor axes. No section demonstrates that these parameters are constrained by any observable other than the anisotropy signal itself (e.g., no radial quenched-fraction profiles, stellar-mass trends, or field-galaxy comparisons at the same epoch are shown to anchor the relative efficiencies). Consequently the reported ~20% major-axis excess may be reproduced by construction once the preprocessing contrast is allowed to vary.

Authors: We thank the referee for highlighting this important point. The parameters in the semi-analytic model are informed by the accretion histories derived from the cosmological simulation, which dictate the timing of infall and the expected alignment with large-scale structure. The preprocessing contrast is physically motivated by the filamentary accretion along the major axis. Nevertheless, we agree that demonstrating consistency with additional observables would better validate the model. In the revised manuscript, we will add comparisons of the model's radial quenched fraction profiles and stellar mass trends to the observed data in our clusters and to field galaxy quenched fractions at similar redshifts from the literature. This will help anchor the relative efficiencies beyond the anisotropy signal alone. revision: yes
Referee: The observational detection is stated to be only ~2σ. Because the central claim that preprocessing dominates and reproduces the anisotropy rests on this marginal signal, the quantitative conclusion that preprocessing accounts for the full observed difference requires a clearer assessment of how the result changes when the significance threshold or sample definition is varied.

Authors: We fully acknowledge that the detection of anisotropic quenching is at a modest ~2σ significance level, as stated in the manuscript. The conclusions are presented with appropriate caution. To provide a clearer assessment of robustness, we will include in the revised manuscript an analysis of how the anisotropy signal varies with different sample definitions, such as restricting to clusters with higher spectroscopic completeness or varying the quiescent galaxy selection criteria. This will allow readers to evaluate the stability of the quantitative conclusions regarding the preprocessing contribution. revision: yes
Referee: The simulation analysis concludes that orientation angles randomize in ~2 Gyr and that only recently accreted galaxies contribute to the anisotropy. It is not shown whether this timescale or the accretion history at z=1.25 remains consistent when the same analysis is repeated on the observed cluster sample or on lower-redshift comparison simulations.

Authors: The accretion history analysis is performed using cosmological simulations at z=1.25 to represent the epoch of our observed clusters (0.9<z<1.4). Repeating the analysis directly on the observed sample is not feasible, as it would require detailed orbital and accretion histories that are not available from observations alone. Regarding lower-redshift simulations, we will add a discussion in the revised version comparing our ~2 Gyr randomization timescale to results from lower-redshift cluster simulations in the literature. We believe this provides the necessary context while recognizing the focus of our study on high-redshift systems. revision: partial

Circularity Check

1 steps flagged · score 6.0 of 10

Semi-analytic model parameterizes intrahalo vs. preprocessing quenching then reproduces observed anisotropy by construction

fitted input called prediction [Abstract]
"We adopt a semi-analytic approach that combines the accretion history of satellite galaxies with a quenching model based on a delay-then-rapid quenching framework and parameterizes both intrahalo quenching and preprocessing effects. We find that preprocessing is the dominant contributor to quenching and that the quenched fraction attributable to preprocessing is higher along the major axis than along the minor axis by ∼20%, reproducing the observed anisotropic quenching signal."

The model is constructed by parameterizing the two channels separately; the subsequent 'finding' that preprocessing dominates and produces a 20% anisotropy that matches the data is the direct output of those parameters. No independent observable is cited to fix the relative efficiencies, so the reported difference is statistically forced once the preprocessing efficiency is allowed to vary.

full rationale

The central claim rests on a semi-analytic model that explicitly parameterizes both quenching channels and is stated to reproduce the ~20% major-axis excess. The accretion histories and ~2 Gyr randomization timescale are taken from simulation, but the relative efficiencies of the two channels have no external anchor shown; the reported dominance and anisotropy therefore reduce to the chosen parameterization rather than an independent prediction.

Assumptions & free parameters 2 free parameters · 2 assumptions · 0 invented entities

The claim depends on the simulation providing accurate recent-accretion fractions and randomization timescales, plus the semi-analytic model's ability to isolate preprocessing without circular tuning to the anisotropy signal itself.

free parameters (2)

quenching delay timescale
Central parameter in the delay-then-rapid framework used to separate intrahalo and preprocessing contributions.
preprocessing efficiency contrast (major vs minor axis)
Parameterized to produce the reported ~20% difference that reproduces the observed signal.

assumptions (2)

domain assumption Satellite orientation angles randomize within ~2 Gyr after accretion
Taken from the z=1.25 simulation analysis and used to argue that only recently infallen galaxies contribute to anisotropy.
domain assumption Majority of satellites in z=1.25 clusters are recently infallen (lesssim 2 Gyr)
Simulation result invoked to link observed anisotropy to preprocessing.

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Cite this review

Pith. "Pith review of Anisotropic quenching beyond $z=1$ and its implications for preprocessing around high-redshift galaxy clusters." pith.science (2026). https://pith.science/paper/QPN5G2BM

@misc{pith2026260623790,
  author       = {Pith},
  title        = {Pith review of: Anisotropic quenching beyond $z=1$ and its implications for preprocessing around high-redshift galaxy clusters},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/QPN5G2BM}},
  note         = {Machine review of arXiv:2606.23790}
}

abstract

Recent studies have shown that, within galaxy clusters, quenched satellite galaxies tend to be distributed preferentially along the major axis of the central galaxy, dubbed anisotropic quenching. There are various discussions about the origin of this anisotropy: some link it to active galactic nucleus activity in the central galaxy, while others attribute it to the preprocessing of galaxies within large-scale structures outside clusters. However, the definitive cause and its redshift dependence remain unclear. In this study, we investigate anisotropic quenching with 12 spectroscopically confirmed galaxy clusters at $0.9<z<1.4$. We calculate the quiescent satellite galaxy fraction as a function of orientation angle measured from the central galaxy's major axis. Although the statistical significance is modest ($\sim 2\sigma$), we detect anisotropic quenching in the highest redshift ever. To understand the origin of the observed anisotropy, we examine the accretion history of satellite galaxies in a cosmological simulation. We find that, in the $z=1.25$ clusters, the majority of satellite galaxies are recently ($\lesssim 2\,\mathrm{Gyr}$) infalled galaxies. In addition, the orientation angles of satellites are randomized immediately after accretion in $\sim 2\,\mathrm{Gyr}$, suggesting that only recently accreted galaxies contribute to the observed anisotropy. We adopt a semi-analytic approach that combines the accretion history of satellite galaxies with a quenching model based on a delay-then-rapid quenching framework and parameterizes both intrahalo quenching and preprocessing effects. We find that preprocessing is the dominant contributor to quenching and that the quenched fraction attributable to preprocessing is higher along the major axis than along the minor axis by $\sim20\%$, reproducing the observed anisotropic quenching signal.

Figures

Figures reproduced from arXiv: 2606.23790 by the authors.

**Figure 1.** Quiescent fraction (fq) as a function of the orientation angle measured from the major axis of central galaxies. Black points are fq calculated in six angular bins, and error bars are from a binomial distribution. The black dashed line shows the median posterior predictions derived from the MCMC realization, while the dark and light yellow shades show the 68% and 95% intervals, respectively. Aq = 0.045 +0.021 0.02… view at source ↗

**Figure 2.** Posterior distributions of Aq and fq,0 from the MCMC fitting for the fiducial model. The median value and 68% credible interval for each parameter are reported at the top. fiducial cosine model is mildly favored. Based on these pieces of evidence, we conclude that the signature of anisotropic quenching in the clusters at z > 1 is confirmed for the first time, although still tentative (2σ level) [PITH_FULL_IMAGE:fig… view at source ↗

**Figure 3.** The normalized histograms of the TSI of the satellite galaxies of TNG300 groups at z = 0 (black dashed line) and z = 1.25 (blue solid line) snapshots. Most satellites of z = 1.25 groups are recent infallers with TSI < ∼ 2Gyr, and only a small fraction of galaxies have TSI > 3Gyr. Note that the sum of the black histogram is not unity since one third of the satellites have TSI > 5Gyr at z = 0 snapshot, and they are n… view at source ↗

Figures from the paper (5 more)

**Figure 4.** Figure 4: Relative orientation angles at a given TSI against the initial values (∆θ = θ(TSI) − θ(TSI = 0)) for satellite galaxies in the TNG simulation at z = 0 (top) and z = 1.25 (bottom). The white solid line represents the median, and the blue shades indicate the 10th to 90th…

**Figure 5.** Figure 5: Same as figure1 but for the semi-analytic quenching modeling. The black dashed line shows the median posterior predictions derived from the MCMC realization, while the dark and light blue areas represent the 68% and 95% intervals, respectively [PITH_FULL_IMAGE:figures…

**Figure 6.** Figure 6: Posterior distributions of four parameters (i.e., τmajor, τminor, fq,pre, ∆fq,pre) of the semi-analytic quenching model derived from MCMC fitting. The median value and 68% credible interval for each parameter are reported at the top. Short quenching timescales (< ∼ 1.5…

**Figure 7.** Figure 7: Fraction of galaxies quenched due to four different pathways in our semi-analytic quenching model: preprocessing along major (orange triangle) and minor (green rectangle) axes, and intrahalo quenching along major (magenta diamond) and minor (blue downward triangle) ax…

**Figure 8.** Figure 8: The relation between orientation angle and TSI for the satellites in the TNG300 groups at z = 1.25. Grey dots represent individual satellites. Blue points indicate their median values and scatters (68% and 90% intervals) in bins with ∆θ = 5 deg. Horizontal black dashe…

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Pith tools

Reviewed June 26, 2026 · model on record in the stance chip above.

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