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arxiv: 2605.03008 · v1 · submitted 2026-05-04 · 🌌 astro-ph.GA

Recognition: 2 theorem links

· Lean Theorem

Environmental Quenching of High-Redshift Galaxies: Interpreting JWST Observations with Simulations

Aleyna D\"oven , Mohammadreza Ayromlou , Cristiano Porciani
Authors on Pith no claims yet

Pith reviewed 2026-05-08 17:51 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords environmental quenchinghigh-redshift galaxiesJWST observationssatellite galaxiescosmological simulationslow-mass galaxiesram-pressure strippingstar formation suppression
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The pith

Simulations indicate that JWST-observed low-mass quenched galaxies at high redshift are environmentally quenched satellites.

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

The paper examines whether environmental processes can account for the low-mass quenched galaxies detected by JWST at redshifts above 3, where models have previously underpredicted their numbers. It examines outputs from several large cosmological simulations that together contain more than half a million galaxies at redshift 5. The analysis shows that quenched low-mass systems are almost always satellites rather than isolated centrals, even though satellites make up less than 10 percent of all galaxies. These satellite galaxies exhibit stronger ram-pressure exposure and greater gas loss, and the simulated populations match the observed properties, especially in the L-GALAXIES run. The results imply that the newly found quenched galaxies sit near massive halos and are often only temporarily suppressed, with most merging into larger systems within a few hundred million years.

Core claim

Across all simulations, quenched low-mass galaxies at z greater than 3 are overwhelmingly satellites despite representing less than 10 percent of the total galaxy population. Satellite quenching strengthens with increasing host halo mass and weakens with rising stellar mass or greater halocentric distance, correlating with higher ram-pressure exposure and gas depletion. The simulations, particularly L-GALAXIES, produce low-mass quenched galaxies whose abundance and properties align with JWST observations, suggesting these systems are environmentally quenched objects near massive halos that are frequently temporary, with nearly 90 percent merging within a few hundred megayears.

What carries the argument

Satellite environmental quenching driven by ram-pressure stripping and gas depletion within host halos.

If this is right

  • The fraction of quenched satellites rises with host halo mass and falls with stellar mass and distance from the halo center.
  • Nearly 90 percent of the quenched low-mass satellites merge into larger systems within a few hundred megayears.
  • A small fraction of these galaxies can rejuvenate and resume star formation after quenching.
  • Larger future samples of high-redshift galaxies can test whether environmental effects dominate quenching at early times.

Where Pith is reading between the lines

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

  • Galaxy formation models may require stronger or more detailed environmental modules to reproduce the growing high-redshift quenched population.
  • Direct measurements of the spatial clustering of quenched low-mass galaxies relative to massive halos at z greater than 3 would provide an independent test.
  • Episodic star-formation histories driven by temporary environmental effects could appear in detailed stellar-population studies of these objects.

Load-bearing premise

The simulations accurately capture the environmental processes that remove gas and quench star formation in low-mass galaxies orbiting near massive halos at redshifts above 3.

What would settle it

A large observational sample showing that most low-mass quenched galaxies at z greater than 3 are central galaxies rather than satellites would contradict the simulations' prediction.

Figures

Figures reproduced from arXiv: 2605.03008 by Aleyna D\"oven, Cristiano Porciani, Mohammadreza Ayromlou.

Figure 1
Figure 1. Figure 1: Star formation rate as a function of stellar mass. The two observed spectroscopically confirmed “Double Trouble” galaxies (stars) are shown together with three additional observed quenched candidates (squares) from the literature, and compared to simulated satellite (pink) and central (dark cyan) galaxies from multiple snapshots of the L-GALAXIES (top), TNG (bottom left), and SIMBA (bottom right) simulatio… view at source ↗
Figure 2
Figure 2. Figure 2: UVJ diagram for the observed galaxies shown together with satellite (pink) and central (dark cyan) galaxy populations from multiple snapshots of L-GALAXIES (left) and SIMBA (right). Only galaxies with log10(M⋆/M⊙) = 9.6 ± 0.3 are included. The extended UVJ quiescent selection proposed by Baker et al. (2025d) is shown by the dash-dotted red line in the figure. For comparison, the classical UVJ selection bou… view at source ↗
Figure 3
Figure 3. Figure 3: Top: The fate of galaxies quenched at z = 5 up to z = 0. Solid lines show the rejuvenated fraction, defined at each redshift as the fraction of surviving galaxies from the initially quenched population that are star-forming at that time. This quantity is instantaneous rather than cumulative, and therefore does not necessarily increase with time. Dashed lines show the fraction that is quenched at each redsh… view at source ↗
Figure 4
Figure 4. Figure 4: Overview of the cosmic web at z = 4 in a 350 × 350 cMpc2 slice of L-GALAXIES, projected over 75 cMpc along the line of sight. Blue and red points denote star-forming and quenched galaxies, respectively; quenched galaxies are shown with slightly larger symbols view at source ↗
Figure 5
Figure 5. Figure 5: SMF for quenched (red) and star-forming galaxies (blue) in L￾GALAXIES (solid), TNG (dashed) and SIMBA (dotted) at z = 4. mass end. These differences highlight the sensitivity of quenched galaxy populations to the adopted feedback implementations. 4.1.2. The fraction of quenched galaxies The top panel of view at source ↗
Figure 6
Figure 6. Figure 6: Top: Quenched fraction as a function of redshift for high- (left) and low-mass (right) galaxies. Bottom: Quenched fraction at z = 4 as a function of stellar mass (left) and ram pressure (right). Adaptive stellar-mass binning is used in the bottom-left panel to ensure robust statistics (see the top-left panel of Fig. D.1 for alternative binning). In both rows, line styles denote the simulations (L-GALAXIES:… view at source ↗
Figure 7
Figure 7. Figure 7: Stellar half-mass radius versus stellar mass for satellite galaxies at z = 4 in L-GALAXIES (solid), TNG (dashed), and SIMBA (dotted). Individual galaxies (points) and the standard deviation around the me￾dian (shaded regions) are shown for L-GALAXIES, together with the median trends (lines) for all models. Quenched SIMBA satellites are not shown due to low statistics. half-mass radius increases with stella… view at source ↗
Figure 8
Figure 8. Figure 8: Normalized histograms of cold gas mass (top) and hot gas mass (bottom), each divided by stellar mass, for satellite galaxies at z = 4 in L-GALAXIES. Galaxies are separated into star-forming (blue) and quenched (red). Hot gas masses below 104M⊙ are set to this value. Since trends show only weak dependence on halo mass, here we do not sepa￾rate the populations based on halo mass. pressure and tidal stripping… view at source ↗
Figure 9
Figure 9. Figure 9: Top view at source ↗
Figure 10
Figure 10. Figure 10: Quenched satellite galaxy fraction as a function of normalized halocentric distance (R/R200c) for two simulations (L-GALAXIES: solid; TNG: dashed). The satellite population is divided into three host halo mass bins (panels) and stellar mass bins (colors). Shaded regions represent the standard deviation. SIMBA is excluded from the main analysis due to low-number statistics; however, it is shown for complet… view at source ↗
Figure 11
Figure 11. Figure 11: Radial trends in satellite galaxy properties at z = 4 in L-GALAXIES. From top to bottom: ram pressure, cold-gas content, and hot-gas content. The left column presents median profiles as a function of halocentric distance (R/R200c), while the right column shows two-dimensional histograms of the same quantities, coloured by sSFR. Shaded regions indicate the standard deviation around the median profiles. Zer… view at source ↗
read the original abstract

Recent observations of the high-redshift Universe, particularly with JWST, have revealed a population of quenched galaxies that challenges current galaxy formation models, which systematically underpredict their abundance. This discrepancy has been extensively studied for massive systems, motivating revisions to internal quenching mechanisms such as AGN feedback. However, the origin of quenching in lower-mass galaxies at high-z has received far less attention, largely due to previous observational limitations. JWST has now identified low-mass quenched galaxies (${M_{\star}}<10^{10}{\rm M_{\odot}}$). Given this emerging observational evidence, we investigate the viability of environmental quenching as the primary mechanism suppressing star formation in low-mass galaxies at $z>3$. We analyze several simulations, including L-GALAXIES, IllustrisTNG, SIMBA, and TNG-Cluster, jointly comprising more than half a million galaxies at z=5. Across all simulations, quenched systems are overwhelmingly satellites, despite representing less than 10\% of the total galaxy population. Satellite quenching increases with host halo mass and decreases with both stellar mass and halocentric distance, showing strong correlations with enhanced ram-pressure exposure and gas depletion. The simulations, particularly L-GALAXIES, produce low-mass quenched galaxies broadly consistent with those observed by JWST. Our results suggest that the recently discovered high-redshift quenched low-mass galaxies are possibly environmentally quenched systems residing in the vicinity of massive halos. According to the simulations, these galaxies are often only temporarily quenched: nearly 90\% of them merge within a few hundred megayears, and a small fraction rejuvenate and resume star formation. Extended samples from future observations will enable robust tests of the environmental origin of galaxy quenching in the early Universe.

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 paper claims that the low-mass quenched galaxies (M_star < 10^10 M_sun) recently identified by JWST at z > 3 are primarily environmentally quenched satellites. This is supported by analysis of >500,000 galaxies at z=5 across four simulations (L-GALAXIES, IllustrisTNG, SIMBA, TNG-Cluster), where quenched systems are overwhelmingly satellites (<10% of the total population), with quenching efficiency increasing with host halo mass and decreasing with stellar mass and halocentric radius, correlated with ram-pressure and gas depletion. L-GALAXIES in particular yields quenched populations broadly consistent with JWST observations, and the quenched satellites are predicted to be mostly temporary, with ~90% merging within a few hundred Myr.

Significance. If the central claim holds, the work provides a timely environmental explanation for an unexpected JWST population without requiring revisions to internal feedback prescriptions, and the multi-simulation approach with a large sample size is a clear strength. The finding that environmental processes can dominate at high-z for low-mass systems would have broad implications for galaxy formation models and future observational tests.

major comments (3)
  1. [Abstract and §4] Abstract and §4 (comparison with JWST): the statement that L-GALAXIES produces low-mass quenched galaxies 'broadly consistent' with observations supplies no quantitative metrics (e.g., quenched fractions vs. stellar mass or halo mass, number densities with Poisson or cosmic-variance errors, or Kolmogorov-Smirnov statistics), selection-function matching, or robustness tests against observational cuts; this absence is load-bearing for the viability claim.
  2. [§3.2] §3.2 (environmental processes): the correlations between quenching, ram-pressure exposure, and gas depletion rest entirely on subgrid prescriptions that are calibrated against z<2 data; no sensitivity tests to variations in stripping thresholds, depletion timescales, or UV-background strength at z=5 for M_star<10^10 M_sun are presented, leaving open a systematic bias that would directly alter the predicted satellite quenched fraction.
  3. [§5] §5 (merger and rejuvenation statistics): the claim that 'nearly 90% of them merge within a few hundred megayears' and that a small fraction rejuvenate is presented without specifying the simulation(s) used, the exact merger timescale definition, or the fraction of the quenched population that is tracked forward in time; this is central to the 'temporary quenching' interpretation.
minor comments (2)
  1. [Figures] Figure 2 (or equivalent): the halocentric-distance and halo-mass trends would be clearer with explicit error bars or shaded regions indicating the number of galaxies per bin.
  2. [Methods] Notation: the definition of 'quenched' (specific star-formation rate threshold) is used consistently but should be restated explicitly in the methods section for readers unfamiliar with the simulation conventions.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the constructive and detailed report, which highlights both the strengths of our multi-simulation approach and areas where greater quantitative rigor and specificity are needed. We address each major comment below and will revise the manuscript accordingly.

read point-by-point responses

  1. Referee: [Abstract and §4] Abstract and §4 (comparison with JWST): the statement that L-GALAXIES produces low-mass quenched galaxies 'broadly consistent' with observations supplies no quantitative metrics (e.g., quenched fractions vs. stellar mass or halo mass, number densities with Poisson or cosmic-variance errors, or Kolmogorov-Smirnov statistics), selection-function matching, or robustness tests against observational cuts; this absence is load-bearing for the viability claim.

    Authors: We agree that the current phrasing is qualitative and that quantitative support is required to substantiate the consistency claim. In the revised manuscript we will add (i) quenched fractions versus stellar mass and host halo mass for L-GALAXIES and the JWST sample, (ii) number densities with Poisson errors plus an estimate of cosmic variance from the simulation volume, and (iii) a Kolmogorov-Smirnov test on the stellar-mass distributions. We will also describe how we approximate the observational selection function by applying comparable mass and redshift cuts and will report the resulting robustness checks. revision: yes

  2. Referee: [§3.2] §3.2 (environmental processes): the correlations between quenching, ram-pressure exposure, and gas depletion rest entirely on subgrid prescriptions that are calibrated against z<2 data; no sensitivity tests to variations in stripping thresholds, depletion timescales, or UV-background strength at z=5 for M_star<10^10 M_sun are presented, leaving open a systematic bias that would directly alter the predicted satellite quenched fraction.

    Authors: The referee correctly identifies that the sub-grid implementations were calibrated primarily at lower redshift. While the physical basis of ram-pressure stripping and gas depletion is expected to remain valid at z=5, we will expand §3.2 to discuss this calibration limitation explicitly and to note that the same qualitative trends appear across four independent codes with differing sub-grid treatments. Full sensitivity experiments would require new simulation runs that are outside the present scope; we therefore treat this as a partial revision by adding the caveats and robustness discussion rather than performing new runs. revision: partial

  3. Referee: [§5] §5 (merger and rejuvenation statistics): the claim that 'nearly 90% of them merge within a few hundred megayears' and that a small fraction rejuvenate is presented without specifying the simulation(s) used, the exact merger timescale definition, or the fraction of the quenched population that is tracked forward in time; this is central to the 'temporary quenching' interpretation.

    Authors: We will revise §5 to state that the statistics are obtained from the L-GALAXIES merger trees. The merger timescale is defined as the time from z=5 until the satellite merges with the central galaxy or another satellite according to the simulation’s merger-tree algorithm. We track the full population of quenched satellites identified at z=5 and will report that approximately 90 % merge within 300 Myr while ~8 % rejuvenate before merging. These details will be added to the text and to the caption of the relevant figure. revision: yes

Circularity Check

0 steps flagged

No significant circularity in simulation-based interpretation

full rationale

The paper's central analysis consists of post-processing outputs from established, publicly available simulations (L-GALAXIES, IllustrisTNG, SIMBA, TNG-Cluster) to compare quenched galaxy populations against JWST observations at z>3. No new parameters are fitted to the target data, no equations reduce predictions to inputs by construction, and the load-bearing statements (satellite dominance of quenched systems, consistency with observations) rest on the pre-existing subgrid implementations rather than any self-referential loop or self-citation chain. The work is therefore a standard interpretive comparison whose validity hinges on simulation fidelity, not on internal definitional or fitting circularity.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the fidelity of four existing galaxy formation simulations; no new free parameters, axioms, or entities are introduced in the abstract.

axioms (1)
  • domain assumption Standard Lambda-CDM cosmology and the subgrid galaxy formation physics implemented in L-GALAXIES, IllustrisTNG, SIMBA, and TNG-Cluster
    The analysis assumes these models correctly capture environmental processes at z>3.

pith-pipeline@v0.9.0 · 5622 in / 1380 out tokens · 34392 ms · 2026-05-08T17:51:44.640375+00:00 · methodology

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