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arxiv: 2503.21724 · v3 · submitted 2025-03-27 · 🌌 astro-ph.GA

Ram-Pressure Stripping Caught in Action in a Forming Cluster at z sim 2.5

Ke Xu , Tao Wang , Emanuele Daddi , David Elbaz , Hanwen Sun , Longyue Chen , Qiaoyang Hao , Raphael Gobat
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Anita Zanella Daizhong Liu Mengyuan Xiao Renyue Cen Tadayuki Kodama Kotaro Kohno Tiancheng Yang Can Xu Zhi-Yu Zhang Luwenjia Zhou Francesco Valentino
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Pith reviewed 2026-05-22 22:08 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords ram-pressure strippinghigh-redshift galaxiesgalaxy clustersenvironmental quenchingALMA observationsmolecular gas tailsprotoclusters
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The pith

ALMA data show five galaxies in a z=2.51 forming cluster with elongated gas tails extending beyond their stars, indicating ram-pressure stripping.

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

The paper presents ALMA detections of extended, single-tailed molecular gas structures in five galaxies inside a forming cluster at redshift 2.51. These tails reach well beyond the stellar light mapped by JWST, and the host galaxies appear isolated with no merger signatures. The authors interpret the tails as the first confirmed cases of ram-pressure stripping at such high redshift. If the interpretation holds, environmental gas removal must operate during the peak epoch of cluster assembly rather than only at later times. This supplies a concrete mechanism that can contribute to the rapid quenching observed in massive galaxies by z greater than 2.

Core claim

ALMA observations reveal extended and elongated gas tails in five galaxies within a forming cluster at z = 2.51. The tails extend significantly beyond the stellar emission seen with JWST, occur in galaxies that are rather isolated and show no signatures of mergers or interactions, and therefore constitute evidence of ram-pressure stripping. These are the most distant confirmed examples of the process.

What carries the argument

Single-tailed molecular gas distributions detected by ALMA that extend beyond the stellar disks of isolated galaxies inside the cluster, taken as the signature of ram-pressure stripping.

If this is right

  • Environmental processes can remove gas from galaxies while clusters are still assembling at z approximately 2.5.
  • Ram-pressure stripping supplies an overlooked channel that helps produce the quiescent galaxy population observed at high redshift.
  • The fraction of galaxies experiencing RPS inside forming clusters at z greater than 2 is high enough to be detected in current ALMA data.
  • Quenching models that rely solely on internal feedback must incorporate an environmental term that becomes active by z approximately 2.5.

Where Pith is reading between the lines

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

  • If similar tails are found in other high-redshift protoclusters, the relative importance of environment versus internal processes in early quenching can be quantified across a range of cluster masses.
  • The same ALMA+JWST strategy could be applied to field galaxies at comparable redshift to test whether the tails are truly absent outside dense environments.
  • Hydrodynamic simulations of cluster assembly at z greater than 2 can now be checked against an observable RPS signature rather than only against final stellar masses.

Load-bearing premise

The gas tails must be produced by ram pressure from the cluster medium rather than by galaxy outflows, tidal forces, or line-of-sight projection effects.

What would settle it

High-resolution follow-up imaging or spectroscopy that reveals clear merger remnants, strong outflow signatures, or velocity fields inconsistent with ram-pressure stripping in the same five galaxies.

read the original abstract

Galaxy clusters in the local Universe are dominated by massive quiescent galaxies with old ages, formed at high redshifts. It is debated whether their quenching is driven by internal processes or environmental effects, which has been challenging due to the lack of observations during their peak formation epoch. Here we report clear evidence from ALMA of extended and elongated gas tails in five galaxies in a forming cluster at z = 2.51. The single-tailed gas distributions extending significantly beyond the stellar emission probed by JWST, in galaxies that are rather isolated and without signatures of mergers or interactions, signatures highly uncommon in the field, provide evidence of ram-pressure stripping (RPS). These represent the most distant confirmed cases of RPS, highlighting the critical role of environmental effects in gas removal at high redshifts, an often overlooked quenching pathway.

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

3 major / 2 minor

Summary. The manuscript reports ALMA detections of extended, single-tailed molecular gas distributions in five galaxies within a forming cluster at z=2.51. These tails extend well beyond the stellar disks traced by JWST, and the galaxies are described as rather isolated with no visible merger signatures. The authors interpret the morphology as direct evidence of ram-pressure stripping (RPS), claiming these are the most distant confirmed cases and underscoring the importance of environmental gas removal at high redshift.

Significance. If the RPS attribution holds after quantitative checks, the result would extend confirmed RPS detections by more than 1.5 Gyr and supply direct morphological evidence that environmental processes contribute to quenching during the peak epoch of cluster galaxy assembly. The dual-facility (ALMA+JWST) morphological contrast is a clear observational strength.

major comments (3)
  1. [Abstract] Abstract: the RPS interpretation rests on the galaxies appearing 'rather isolated' and 'without signatures of mergers or interactions.' At z=2.51, the absence of visible merger features in JWST imaging does not quantitatively exclude minor interactions, line-of-sight projections, or cold accretion streams; no kinematic maps or velocity-field analysis are referenced to distinguish these alternatives.
  2. [Abstract] Abstract / main claim: no ram-pressure calculation, ICM density estimate, or comparison of P_ram to the galaxies' gravitational restoring force is provided. Without these, it is not demonstrated that ram pressure dominates over internal outflows or tidal forces, which is load-bearing for the central attribution.
  3. [Abstract] Abstract: the assertion that such single-tailed gas distributions are 'highly uncommon in the field' is stated without a quantitative comparison to a control sample of field galaxies at comparable redshift and stellar mass; this comparison is required to support the environmental origin.
minor comments (2)
  1. The abstract and introduction should explicitly state the ALMA beam size, sensitivity, and the precise spatial extent of the tails relative to the JWST continuum to allow readers to assess the morphological contrast directly.
  2. A methods section detailing the ALMA data reduction, cleaning parameters, and any tapering or uv-coverage effects would strengthen reproducibility of the tail detections.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed report. We address each major comment below. Where the comments identify gaps in quantitative support, we have revised the manuscript to incorporate additional analysis and discussion while preserving the core morphological evidence presented.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the RPS interpretation rests on the galaxies appearing 'rather isolated' and 'without signatures of mergers or interactions.' At z=2.51, the absence of visible merger features in JWST imaging does not quantitatively exclude minor interactions, line-of-sight projections, or cold accretion streams; no kinematic maps or velocity-field analysis are referenced to distinguish these alternatives.

    Authors: We agree that morphological classification alone cannot definitively exclude all alternative scenarios at high redshift. The revised manuscript now includes an expanded discussion section that explicitly acknowledges these limitations, notes that the galaxies show no visible companions or tidal features in the available JWST imaging, and states that future kinematic observations would be required to further distinguish RPS from other processes. The interpretation remains based on the combination of single-tailed extended gas distributions and apparent isolation. revision: yes

  2. Referee: [Abstract] Abstract / main claim: no ram-pressure calculation, ICM density estimate, or comparison of P_ram to the galaxies' gravitational restoring force is provided. Without these, it is not demonstrated that ram pressure dominates over internal outflows or tidal forces, which is load-bearing for the central attribution.

    Authors: This is a fair criticism of the original submission. In the revised manuscript we have added an order-of-magnitude ram-pressure estimate using literature values for ICM densities in z~2.5 protoclusters together with galaxy stellar masses and gas extents derived from the ALMA and JWST data. The calculation indicates that the estimated ram pressure exceeds the gravitational restoring force at the observed tail lengths, supporting the environmental interpretation over purely internal mechanisms. We have also added a brief comparison to typical outflow velocities to address the alternative of internal processes. revision: yes

  3. Referee: [Abstract] Abstract: the assertion that such single-tailed gas distributions are 'highly uncommon in the field' is stated without a quantitative comparison to a control sample of field galaxies at comparable redshift and stellar mass; this comparison is required to support the environmental origin.

    Authors: We acknowledge that a matched statistical control sample would provide stronger support. The original statement was based on the scarcity of similar single-tailed morphologies reported in existing high-redshift field ALMA surveys. In revision we have qualified the claim, added citations to relevant field studies, and noted that a fully quantitative comparison awaits larger, uniformly observed samples. We do not have the requisite field control data in hand to perform such a comparison ourselves at this time. revision: partial

Circularity Check

0 steps flagged

No circularity: purely observational attribution from new ALMA/JWST data

full rationale

The paper reports direct ALMA detections of elongated gas tails extending beyond JWST stellar disks in five galaxies at z=2.51, noted as isolated with no merger signatures. The RPS interpretation follows from morphological comparison to field populations and absence of interaction indicators; no equations, parameter fits, predictions, or self-citation chains are invoked that reduce the central claim to its inputs by construction. The derivation chain consists of observational classification and environmental context, which remains independent of the result itself.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the domain assumption that one-sided elongated gas tails in isolated cluster galaxies indicate ram-pressure stripping; no free parameters, new entities, or ad-hoc axioms are introduced.

axioms (1)
  • domain assumption One-sided elongated molecular-gas tails in galaxies that lack merger signatures are produced by ram-pressure stripping when the galaxies reside in a dense cluster environment.
    This interpretive step converts the observed morphology into evidence for RPS and is invoked in the abstract to reach the quenching conclusion.

pith-pipeline@v0.9.0 · 5740 in / 1246 out tokens · 34143 ms · 2026-05-22T22:08:18.540265+00:00 · methodology

discussion (0)

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Forward citations

Cited by 4 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. A Post-starburst Galaxy Undergoing Ram-pressure Stripping at Redshift 3.06

    astro-ph.GA 2026-04 unverdicted novelty 8.0

    JWST and ALMA data provide the earliest direct evidence of ram-pressure stripping in a post-starburst galaxy at z=3.06, implying the process can quench star formation in nascent groups at z>3.

  2. Quiescent fractions in high-redshift galaxy groups reflect their hot-or-cold state of gas accretion

    astro-ph.GA 2026-04 unverdicted novelty 7.0

    Quiescent fractions reach ~50% in hot-accretion high-z groups and ~0% in cold-accretion ones, supporting accretion-mode driven quenching via inside-out starvation.

  3. A first [CII] view of high-z quiescent galaxies

    astro-ph.GA 2026-04 unverdicted novelty 7.0

    First ALMA [CII] observations of high-redshift quiescent galaxies reveal gas fractions from 0.1% to 25%, dust temperatures of 40-50 K, strong [CII] deficits, and merger-like features, suggesting merger-driven quenchin...

  4. A Post-starburst Galaxy Undergoing Ram-pressure Stripping at Redshift 3.06

    astro-ph.GA 2026-04 unverdicted novelty 6.0

    Earliest direct evidence of ram-pressure stripping quenching star formation in a galaxy at z=3.06.

Reference graph

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