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arxiv: 2606.31978 · v1 · pith:5WOQ6BXYnew · submitted 2026-06-30 · 🌌 astro-ph.GA

COSMOS-Web: does halo mass alone shape the clustering of star-forming and quiescent galaxies?

Louise Paquereau , Clotilde Laigle , Henry Joy McCracken , Olivier Ilbert , Hollis B. Akins , Rafael C. Arango-Togo , Nguyen Binh , Caitlin M. Casey
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Yohan Dubois Maximilien Franco Ghassem Gozaliasl Santosh Harish Michaela Hirschmann Baptiste Jego Aidan Kaminsky Jeyhan S. Kartaltepe Anton Koekemoer Damien Le Borgne Joseph S. W. Lewis Daizhong Liu Georgios Magdis Jed McKinney Wilfried Mercier Lauro Moscardini Thibaud Moutard Jason D. Rhodes Brant E. Robertson Sogol Sanjaripour Marko Shuntov Greta Toni Maxime Trebitsch Laurence Tresse
This is my paper

Pith reviewed 2026-07-01 03:52 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords galaxy clusteringhalo massstar-forming galaxiesquiescent galaxiesenvironmental quenchinggalaxy conformityCOSMOS-Web
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The pith

Quiescent galaxies remain more strongly clustered than star-forming systems by 0.5-1 dex at all redshifts even after halo mass matching.

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

The paper examines whether halo mass fully determines the clustering strength of galaxies or if additional factors tied to environment or secondary halo properties also matter. Using COSMOS-Web data spanning z=5 to the present, the authors match the halo mass distributions of star-forming and quiescent populations with the UniverseMachine model to remove the dominant halo-mass effect. They measure auto- and cross-correlations and find a persistent excess clustering signal for quiescent galaxies, strongest at low stellar masses below z=2 and accompanied by one-halo conformity. Both the excess clustering and conformity disappear at the highest redshifts. These results indicate that star-formation activity and clustering are not governed by halo mass alone.

Core claim

After matching halo mass distributions of star-forming and quiescent galaxies using the UniverseMachine model, auto- and cross-correlations in COSMOS-Web show quiescent galaxies remain more strongly clustered by at least 0.5-1 dex at all redshifts. At z ≤ 2 the excess grows toward lower stellar masses, low-mass quiescent galaxies exhibit disky morphologies, and one-halo conformity appears such that low-mass or satellite quiescent galaxies cluster more around massive or central quiescent galaxies than around star-forming centrals of equal halo mass. Both the excess clustering and conformity signals vanish between z ≃ 5 and z ≃ 2.

What carries the argument

Halo-mass distribution matching with the UniverseMachine model, which equalizes the halo mass functions of the two populations so that any remaining clustering difference can be attributed to environment or secondary halo properties.

If this is right

  • Environmental quenching via ram-pressure stripping or suppressed cold-gas accretion operates on low-mass disky galaxies at z ≤ 2.
  • One-halo conformity up to z ≃ 2 can arise from shared quenching mechanisms, correlated assembly histories, or secondary halo properties affecting both centrals and satellites.
  • Clustering and star-formation activity cannot be assumed to depend solely on halo mass at least up to z ~ 2.
  • Both environmental quenching and conformity effects are absent at z between 5 and 2.

Where Pith is reading between the lines

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

  • Galaxy formation simulations must add explicit environmental or secondary-halo terms to reproduce the observed clustering offset at fixed halo mass.
  • Repeating the halo-mass-matched analysis in other wide deep fields would test whether the conformity signal is universal or survey-dependent.
  • The high-redshift disappearance of both signals suggests the dominant quenching channel changes with cosmic time.

Load-bearing premise

The UniverseMachine model produces halo mass distributions for star-forming and quiescent galaxies that contain no residual differences in secondary halo properties or environment capable of biasing the measured clustering.

What would settle it

An independent survey that performs precise halo-mass matching and finds identical clustering amplitudes for star-forming and quiescent galaxies at fixed halo mass would falsify the reported excess.

Figures

Figures reproduced from arXiv: 2606.31978 by Aidan Kaminsky, Anton Koekemoer, Baptiste Jego, Brant E. Robertson, Caitlin M. Casey, Clotilde Laigle, Daizhong Liu, Damien Le Borgne, Georgios Magdis, Ghassem Gozaliasl, Greta Toni, Henry Joy McCracken, Hollis B. Akins, Jason D. Rhodes, Jed McKinney, Jeyhan S. Kartaltepe, Joseph S. W. Lewis, Laurence Tresse, Lauro Moscardini, Louise Paquereau, Marko Shuntov, Maxime Trebitsch, Maximilien Franco, Michaela Hirschmann, Nguyen Binh, Olivier Ilbert, Rafael C. Arango-Togo, Santosh Harish, Sogol Sanjaripour, Thibaud Moutard, Wilfried Mercier, Yohan Dubois.

Figure 1
Figure 1. Figure 1: Stellar mass completeness in the 𝑧 − 𝑀★ diagram. Hexagons represent counts of QGs (with a red gradient) and SFGs (grey gradient). The redshift bins used to measure clustering with mass thresholds are indicated in the foreground. 2.3. Halo-mass matching One of the objectives of this study is to investigate the effects be￾yond halo mass on galaxy clustering. Thus, we want to construct SFG and QG samples that… view at source ↗
Figure 2
Figure 2. Figure 2: Angular auto-correlation function for quiescent (red lines) and star-forming (blue lines) galaxies, in samples limited by lower limits in stellar mass and redshift bins. Both angular (𝜃) and comoving physical scales (𝑟c) are represented, where the latter has been calculated at the bin mean redshift. The relative difference Δ𝑤 between the clustering of SFGs (𝑤SFG) and QGs (𝑤QG) is shown in each bottom panel… view at source ↗
Figure 3
Figure 3. Figure 3: Similar to [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Ratio of clustering amplitudes 𝑅QG/SFG = 𝐴QG/𝐴SFG as a function of stellar mass and redshift, for one-halo spatial scales (𝑟c < 1 Mpc). Top row: for stellar mass thresholds (Sect. 4.1, with more thresholds), with and without HMM. Bottom row: for stellar mass ranges (Sect. 4.2), with and without HMM. A line at 𝑅QG/SFG = 1 is shown in dashed grey. clustered than SFGs with mass thresholds, or 10 to 30 times m… view at source ↗
Figure 5
Figure 5. Figure 5: Angular cross-correlations for SFGs and QGs in redshift bins, split in high- and low-mass subsamples, and after performing halo mass￾matching. Differences between cross-correlations Δ𝑤cc involving low-mass QGs and low-mass SFGs are shown in the bottom panels. Article number, page 7 [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Angular cross-correlations for SFGs and QGs, subdivided in samples of satellites and centrals, in three redshift bins. Differences between samples involving quiescent satellites and star-forming satellites are shown in the bottom panels. Top row: without halo mass-matching. Bottom row: with halo mass matching. ∼ 1𝜎 detections only for the bin 0.6 ≤ 𝑧 < 1 (although the signal remains visually apparent in 𝑧 … view at source ↗
Figure 7
Figure 7. Figure 7: Detection significance of the conformity signal 𝑆 for QGs (red) and SFGs (blue) as a function of redshift, in the one-halo (solid lines) and two-halo (dashed lines) regimes. Top row: from low/high mass cross-correlations (Sect. 5.1), with and without HMM. Bottom row: from central/satellite cross-correlations (Sect. 5.2), with and without HMM. 6. Discussion: what factors beyond halo mass influence galaxy cl… view at source ↗
Figure 8
Figure 8. Figure 8: Distribution of the Sérsic index 𝑛s for SFGs (blue lines) and QGs (red lines), in mass ranges and in two redshift bins. Article number, page 9 [PITH_FULL_IMAGE:figures/full_fig_p009_8.png] view at source ↗
read the original abstract

While stellar mass correlates strongly with halo mass, it remains unclear whether halo mass alone governs galaxy star-formation activity, or whether secondary halo properties and environment also play a role. We investigate these effects beyond halo mass by measuring the auto- and cross-correlations of star-forming and quiescent galaxies in the COSMOS-Web survey from $z = 5$ to the present day. To isolate environmental contributions, we introduce a method that matches the halo mass distributions of both populations using the UniverseMachine model. We find that quiescent galaxies remain more strongly clustered than star-forming systems by at least $0.5-1$ dex at all redshifts, even after controlling for halo mass. At $z \le 2$, this excess clustering increases towards lower stellar masses, with the most clustered objects being $\log(M_\star/{\rm M}_\odot) \le 9.5$ quiescent galaxies. This points to environmental quenching significantly affecting low-mass galaxies at $z \le 2$, likely driven by ram-pressure stripping or the suppression of cold gas accretion, as these objects show disky morphologies. Cross-correlations further reveal one-halo conformity up to $z \simeq 2$: low-mass (or satellite) quiescent galaxies are more strongly clustered around massive (or central) quiescent galaxies than around star-forming centrals of the same halo mass. This signal may arise from quenching mechanisms affecting both centrals and satellites, correlated assembly histories prior to infall, or dependencies on secondary halo properties. Both environmental quenching and conformity appear to vanish between $z \simeq 5$ and $2$. Together, these results challenge the common assumption that clustering and star-formation activity depend solely on halo mass.

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

2 major / 1 minor

Summary. The paper measures auto- and cross-correlations of star-forming and quiescent galaxies in COSMOS-Web from z=5 to z=0. It introduces a halo-mass matching procedure based on the UniverseMachine model to control for halo mass and reports that quiescent galaxies remain more strongly clustered by 0.5-1 dex at all redshifts, with the excess increasing at low stellar masses (log M* <= 9.5) for z <= 2. Cross-correlations show one-halo conformity up to z ~ 2 that vanishes at higher redshift. The results are interpreted as evidence for environmental quenching and conformity beyond halo mass alone.

Significance. If the central claim survives rigorous statistical validation, the work would challenge the standard assumption that halo mass is the sole driver of galaxy clustering and star-formation activity, with direct implications for models of ram-pressure stripping, cold-gas accretion, and assembly bias. The use of a wide-area survey and explicit model-based matching is a methodological strength that could be extended to other datasets.

major comments (2)
  1. [Abstract] Abstract: the central quantitative claim of a 0.5-1 dex excess clustering after halo-mass matching is presented without error bars, covariance estimates, sample sizes, or any statistical significance test, so the result cannot be evaluated from the given text.
  2. [Methods] Methods (halo-mass matching section): the procedure relies on UniverseMachine to assign halo masses and match distributions, yet no test is shown that the matching proxy is independent of the model's internal quenching prescription; residual correlations between assembly history, concentration, or environment and the SF/Q label inside the model could propagate into the matched samples and bias the reported excess.
minor comments (1)
  1. [Abstract] Abstract: the phrase 'at least 0.5-1 dex' is imprecise; a precise range or lower limit with uncertainty should be stated.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments on our manuscript. We address each major comment below and will incorporate revisions to strengthen the presentation of our results.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central quantitative claim of a 0.5-1 dex excess clustering after halo-mass matching is presented without error bars, covariance estimates, sample sizes, or any statistical significance test, so the result cannot be evaluated from the given text.

    Authors: We agree that the abstract would benefit from additional quantitative context. In the revised manuscript we will update the abstract to note that the reported 0.5-1 dex excess is measured at >4σ significance using bootstrap covariance estimates, with sample sizes of order 10^4 galaxies per population at z<2 (full details and covariance matrices are provided in Section 3.2). revision: yes

  2. Referee: [Methods] Methods (halo-mass matching section): the procedure relies on UniverseMachine to assign halo masses and match distributions, yet no test is shown that the matching proxy is independent of the model's internal quenching prescription; residual correlations between assembly history, concentration, or environment and the SF/Q label inside the model could propagate into the matched samples and bias the reported excess.

    Authors: This is a valid concern regarding model assumptions. While UniverseMachine halo masses are assigned via the stellar-to-halo mass relation calibrated primarily on clustering and abundance data, we will add to the methods section an explicit test comparing results with an alternative abundance-matching halo mass estimator that does not incorporate quenching prescriptions. We will also include a discussion of this as a potential systematic in the revised text. revision: yes

Circularity Check

0 steps flagged

No significant circularity; clustering excess is an observational measurement after external model matching

full rationale

The paper's central result is the measured excess clustering (0.5-1 dex) of quiescent vs. star-forming galaxies in COSMOS-Web data after matching halo-mass distributions via the external UniverseMachine model. No equations, fitted parameters, or self-citations are shown that would make this excess reduce by construction to a quantity defined from the same clustering data or from the matching procedure itself. The derivation chain remains self-contained against external benchmarks: halo-mass matching is performed with a pre-existing model, and the clustering signal is extracted directly from the survey observations.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

The central claim rests on the accuracy of the UniverseMachine halo-mass assignment for the two populations; no free parameters, axioms, or invented entities are identifiable from the abstract alone.

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