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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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Reference graph

Works this paper leans on

300 extracted references · 290 canonical work pages · 131 internal anchors

  1. [1]

    , keywords =

    Tracing the galaxy-halo connection with galaxy clustering in COSMOS-Web from z = 0.1 to z 12. , keywords =. doi:10.1051/0004-6361/202553828 , archivePrefix =. 2501.11674 , primaryClass =

    work page doi:10.1051/0004-6361/202553828

  2. [2]

    Annual Review of Nuclear and Particle Science , keywords =

    Weak Gravitational Lensing and Its Cosmological Applications. Annual Review of Nuclear and Particle Science , keywords =. doi:10.1146/annurev.nucl.58.110707.171151 , archivePrefix =. 0805.0139 , primaryClass =

    work page doi:10.1146/annurev.nucl.58.110707.171151

  3. [3]

    arXiv e-prints , keywords =

    Large Scale Structure and the Cosmic Web. arXiv e-prints , keywords =. doi:10.48550/arXiv.2503.21759 , archivePrefix =. 2503.21759 , primaryClass =

    work page doi:10.48550/arxiv.2503.21759

  4. [4]

    arXiv e-prints , keywords =

    Mergers of galaxies. arXiv e-prints , keywords =. doi:10.48550/arXiv.2506.09136 , archivePrefix =. 2506.09136 , primaryClass =

    work page doi:10.48550/arxiv.2506.09136

  5. [5]

    Green Valley Galaxies

    Green Valley Galaxies. Serbian Astronomical Journal , keywords =. doi:10.2298/SAJ1489001S , archivePrefix =. 1501.01963 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.2298/saj1489001s

  6. [6]

    Weak lensing for precision cosmology

    Weak Lensing for Precision Cosmology. , keywords =. doi:10.1146/annurev-astro-081817-051928 , archivePrefix =. 1710.03235 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-081817-051928

  7. [7]

    Gas Accretion and Angular Momentum

    Gas Accretion and Angular Momentum. Gas Accretion onto Galaxies , year = 2017, editor =. doi:10.1007/978-3-319-52512-9_11 , archivePrefix =. 1612.00513 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/978-3-319-52512-9_11 2017

  8. [8]

    , keywords =

    Radio galaxies and feedback from AGN jets. , keywords =. doi:10.1016/j.newar.2020.101539 , archivePrefix =. 2003.06137 , primaryClass =

    work page doi:10.1016/j.newar.2020.101539 2020

  9. [9]

    Large-Scale Structure of the Universe and Cosmological Perturbation Theory

    Large-scale structure of the Universe and cosmological perturbation theory. , keywords =. doi:10.1016/S0370-1573(02)00135-7 , archivePrefix =. astro-ph/0112551 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/s0370-1573(02)00135-7

  10. [10]

    The Cosmological Constant

    The Cosmological Constant. Living Reviews in Relativity , keywords =. doi:10.12942/lrr-2001-1 , archivePrefix =. astro-ph/0004075 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.12942/lrr-2001-1 2001

  11. [11]

    , keywords =

    Challenges for CDM: An update. , keywords =. doi:10.1016/j.newar.2022.101659 , archivePrefix =. 2105.05208 , primaryClass =

    work page doi:10.1016/j.newar.2022.101659 2022

  12. [12]

    Theoretical Challenges in Galaxy Formation

    Theoretical Challenges in Galaxy Formation. , keywords =. doi:10.1146/annurev-astro-081913-040019 , archivePrefix =. 1612.06891 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-081913-040019

  13. [13]

    , keywords =

    The Dawes Review 10: The impact of deep learning for the analysis of galaxy surveys. , keywords =. doi:10.1017/pasa.2022.55 , archivePrefix =. 2210.01813 , primaryClass =

    work page doi:10.1017/pasa.2022.55 2022

  14. [14]

    and Mead, A

    The halo model for cosmology: a pedagogical review. The Open Journal of Astrophysics , keywords =. doi:10.21105/astro.2303.08752 , archivePrefix =. 2303.08752 , primaryClass =

    work page doi:10.21105/astro.2303.08752

  15. [15]

    Physical Properties of Galaxies from z=2-4

    Physical Properties of Galaxies from z = 2-4. , keywords =. doi:10.1146/annurev-astro-081710-102542 , archivePrefix =. 1107.5060 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-081710-102542

  16. [16]

    , keywords =

    The [O III]+H equivalent width distribution at z ≃ 7: implications for the contribution of galaxies to reionization. , keywords =. doi:10.1093/mnras/staa3370 , archivePrefix =. 2005.02402 , primaryClass =

    work page doi:10.1093/mnras/staa3370 2005

  17. [17]

    The Frontier Fields: Survey Design

    The Frontier Fields: Survey Design and Initial Results. , keywords =. doi:10.3847/1538-4357/837/1/97 , archivePrefix =. 1605.06567 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/837/1/97

  18. [18]

    , keywords =

    Insight from JWST/Near Infrared Camera into galaxy overdensities around bright Lyman-alpha emitters during reionization: implications for ionized bubbles at z 9. , keywords =. doi:10.1093/mnras/stae516 , archivePrefix =. 2305.16670 , primaryClass =

    work page doi:10.1093/mnras/stae516

  19. [19]

    The Universe is Reionizing at z~7: Bayesian Inference of the IGM Neutral Fraction Using Ly$\alpha$ Emission from Galaxies

    The Universe Is Reionizing at z 7: Bayesian Inference of the IGM Neutral Fraction Using Ly Emission from Galaxies. , keywords =. doi:10.3847/1538-4357/aab0a7 , archivePrefix =. 1709.05356 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aab0a7

  20. [20]

    Spectroscopic Constraints on UV Metal Line Emission at z~6-9: The Nature of Lyman-alpha Emitting Galaxies in the Reionization-Era

    Spectroscopic constraints on UV metal line emission at z ≃ 6-9: the nature of Ly emitting galaxies in the reionization era. , keywords =. doi:10.1093/mnras/sty1640 , archivePrefix =. 1804.00041 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty1640

  21. [21]

    , keywords =

    The Detection of Ionized Carbon Emission at z 8. , keywords =. doi:10.3847/2041-8213/ac1a79 , archivePrefix =. 2107.06295 , primaryClass =

    work page doi:10.3847/2041-8213/ac1a79 2041

  22. [22]

    , keywords =

    Hubble Space Telescope/Advanced Camera for Surveys Morphology of Ly Emitters at Redshift 5.7 in the COSMOS Field. , keywords =. doi:10.1088/0004-637X/701/2/915 , adsurl =

    work page doi:10.1088/0004-637x/701/2/915

  23. [23]

    , year = 1967, month = mar, volume =

    Are Young Galaxies Visible?. , year = 1967, month = mar, volume =. doi:10.1086/149079 , adsurl =

    work page doi:10.1086/149079 1967

  24. [24]

    A Galaxy at z=5.34

    A Galaxy at z = 5.34. , keywords =. doi:10.1086/311331 , archivePrefix =. astro-ph/9803137 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/311331

  25. [25]

    Systematic Identification of LAEs for Visible Exploration and Reionization Research Using Subaru HSC (SILVERRUSH). I. Program strategy and clustering properties of 2000 Ly emitters at z = 6-7 over the 0.3-0.5 Gpc ^ 2 survey area. , keywords =. doi:10.1093/pasj/psx074 , archivePrefix =. 1704.07455 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/pasj/psx074 2000

  26. [26]

    , year = 2020, volume =

    Observations of the Lyman- Universe. , keywords =. doi:10.1146/annurev-astro-032620-021859 , archivePrefix =. 2012.07960 , primaryClass =

    work page doi:10.1146/annurev-astro-032620-021859 2012

  27. [27]

    , keywords =

    The First Stars: Formation, Properties, and Impact. , keywords =. doi:10.1146/annurev-astro-071221-053453 , archivePrefix =. 2303.12500 , primaryClass =

    work page doi:10.1146/annurev-astro-071221-053453

  28. [28]

    , keywords =

    Galaxy Formation and Reionization: Key Unknowns and Expected Breakthroughs by the James Webb Space Telescope. , keywords =. doi:10.1146/annurev-astro-120221-044656 , archivePrefix =. 2110.13160 , primaryClass =

    work page doi:10.1146/annurev-astro-120221-044656

  29. [29]

    , keywords =

    Small-Scale Challenges to the CDM Paradigm. , keywords =. doi:10.1146/annurev-astro-091916-055313 , archivePrefix =. 1707.04256 , primaryClass =

    work page doi:10.1146/annurev-astro-091916-055313

  30. [30]

    The Evolution of Galaxy Structure over Cosmic Time

    The Evolution of Galaxy Structure Over Cosmic Time. , keywords =. doi:10.1146/annurev-astro-081913-040037 , archivePrefix =. 1403.2783 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-081913-040037

  31. [31]

    The Connection between Galaxies and their Dark Matter Halos

    The Connection Between Galaxies and Their Dark Matter Halos. , keywords =. doi:10.1146/annurev-astro-081817-051756 , archivePrefix =. 1804.03097 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-081817-051756

  32. [32]

    Encyclopedia of Astrophysics, Volume 4 , year = 2026, volume =

    Observations of the first galaxies in the Era of JWST. Encyclopedia of Astrophysics, Volume 4 , year = 2026, volume =. doi:10.1016/B978-0-443-21439-4.00128-0 , archivePrefix =. 2501.17078 , primaryClass =

    work page doi:10.1016/b978-0-443-21439-4.00128-0 2026

  33. [33]

    Halo Models of Large Scale Structure

    Halo models of large scale structure. , keywords =. doi:10.1016/S0370-1573(02)00276-4 , archivePrefix =. astro-ph/0206508 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/s0370-1573(02)00276-4

  34. [34]

    doi:10.1515/9780691206721 , adsurl =

    Principles of Physical Cosmology. doi:10.1515/9780691206721 , adsurl =

    work page doi:10.1515/9780691206721

  35. [35]

    doi:10.1017/CBO9780511807244 , adsurl =

    Galaxy Formation and Evolution. doi:10.1017/CBO9780511807244 , adsurl =

    work page doi:10.1017/cbo9780511807244

  36. [36]

    Malicious User Experience Design Research for Cybersecurity

    Theory of Star Formation. , keywords =. doi:10.1146/annurev.astro.45.051806.110602 , archivePrefix =. 0707.3514 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev.astro.45.051806.110602

  37. [37]

    Notes on Star Formation

    Notes on Star Formation. arXiv e-prints , keywords =. doi:10.48550/arXiv.1511.03457 , archivePrefix =. 1511.03457 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1511.03457

  38. [38]

    Physical Models of Galaxy Formation in a Cosmological Framework

    Physical Models of Galaxy Formation in a Cosmological Framework. , keywords =. doi:10.1146/annurev-astro-082812-140951 , archivePrefix =. 1412.2712 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-082812-140951

  39. [39]

    The impact of cosmic filaments on starburst galaxies across cosmic times

    The impact of cosmic filaments on starburst galaxies across cosmic times. arXiv e-prints , keywords =. doi:10.48550/arXiv.2602.21890 , archivePrefix =. 2602.21890 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2602.21890

  40. [40]

    , keywords =

    Large-scale Structure in COSMOS-Web: Tracing Galaxy Evolution in the Cosmic Web up to z 7 with the Largest JWST Survey. , keywords =. doi:10.3847/1538-4357/ae5bac , archivePrefix =. 2511.10727 , primaryClass =

    work page doi:10.3847/1538-4357/ae5bac

  41. [41]

    COSMOS-Web galaxy groups: Evolution of red sequence and quiescent galaxy fraction

    COSMOS-Web galaxy groups: Evolution of red sequence and quiescent galaxy fraction. , keywords =. doi:10.1051/0004-6361/202557183 , archivePrefix =. 2509.08040 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202557183

  42. [42]

    Molecular gas properties of star-forming brightest group galaxies at $z \sim 0.3$

    Molecular gas properties of star-forming brightest group galaxies at z 0.3. arXiv e-prints , keywords =. doi:10.48550/arXiv.2605.21592 , archivePrefix =. 2605.21592 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2605.21592

  43. [43]

    Nature Astronomy , keywords =

    An ultra-high-resolution map of (dark) matter. Nature Astronomy , keywords =. doi:10.1038/s41550-025-02763-9 , archivePrefix =. 2601.17239 , primaryClass =

    work page doi:10.1038/s41550-025-02763-9

  44. [44]

    , keywords =

    Deep Realistic Extragalactic Model (DREaM) Galaxy Catalogs: Predictions for a Roman Ultra-deep Field. , keywords =. doi:10.3847/1538-4357/ac46fb , archivePrefix =. 2110.10703 , primaryClass =

    work page doi:10.3847/1538-4357/ac46fb

  45. [45]

    The Spitzer Legacy Survey of the HST-ACS 2 sq. deg. COSMOS Field: survey strategy and first analysis

    S-COSMOS: The Spitzer Legacy Survey of the Hubble Space Telescope ACS 2 deg ^ 2 COSMOS Field I: Survey Strategy and First Analysis. , keywords =. doi:10.1086/517885 , archivePrefix =. astro-ph/0701318 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/517885

  46. [46]

    The Chandra COSMOS Legacy survey: optical/IR identifications

    The Chandra COSMOS Legacy survey: optical/IR identifications. , keywords =. doi:10.3847/0004-637X/817/1/34 , archivePrefix =. 1512.01105 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/817/1/34

  47. [47]

    Survey strategy, observations, and sample properties of 118 star-forming galaxies at 4 < z < 6

    The ALPINE-ALMA [CII] survey. Survey strategy, observations, and sample properties of 118 star-forming galaxies at 4 < z < 6. , keywords =. doi:10.1051/0004-6361/201936965 , archivePrefix =. 1910.09517 , primaryClass =

    work page doi:10.1051/0004-6361/201936965 1910

  48. [48]

    The First Release COSMOS Optical and Near-IR Data and Catalog

    The First Release COSMOS Optical and Near-IR Data and Catalog. , keywords =. doi:10.1086/519081 , archivePrefix =. 0704.2430 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/519081

  49. [49]

    , keywords =

    Brightest group galaxies in COSMOS-Web: Evolution of the size-mass relation since z = 3.7. , keywords =. doi:10.1051/0004-6361/202556085 , archivePrefix =. 2506.04031 , primaryClass =

    work page doi:10.1051/0004-6361/202556085

  50. [50]

    , keywords =

    COSMOS-Web: MIRI Data Reduction and Number Counts at 7.7 m Using JWST. , keywords =. doi:10.3847/1538-4357/adfa1e , archivePrefix =. 2506.03306 , primaryClass =

    work page doi:10.3847/1538-4357/adfa1e

  51. [51]

    , keywords =

    COSMOS-Web: Comprehensive Data Reduction for Wide-area JWST NIRCam Imaging. , keywords =. doi:10.3847/1538-4357/ae3aa1 , archivePrefix =. 2506.03256 , primaryClass =

    work page doi:10.3847/1538-4357/ae3aa1

  52. [52]

    B., Paquereau, L., et al

    COSMOS2025: The COSMOS-Web galaxy catalog of photometry, morphology, redshifts, and physical parameters from JWST, HST, and ground-based imaging. , keywords =. doi:10.1051/0004-6361/202555799 , archivePrefix =. 2506.03243 , primaryClass =

    work page doi:10.1051/0004-6361/202555799

  53. [53]

    , keywords =

    Testing for Intrinsic Type Ia Supernova Luminosity Evolution at z > 2 with JWST. , keywords =. doi:10.3847/2041-8213/adb1d9 , archivePrefix =. 2411.11953 , primaryClass =

    work page doi:10.3847/2041-8213/adb1d9 2041

  54. [54]

    , keywords =

    Tracing High-z Galaxies in X-Rays with JWST and Chandra. , keywords =. doi:10.3847/1538-4357/adcede , archivePrefix =. 2502.09705 , primaryClass =

    work page doi:10.3847/1538-4357/adcede

  55. [55]

    , keywords =

    Going deeper into the dark with COSMOS-Web: JWST unveils the total contribution of radio-selected NIR-faint galaxies to the cosmic star formation rate density. , keywords =. doi:10.1051/0004-6361/202452461 , archivePrefix =. 2503.00112 , primaryClass =

    work page doi:10.1051/0004-6361/202452461

  56. [56]

    , keywords =

    Not-so-little Red Dots: Two Massive and Dusty Starbursts at z 5 7 Pushing the Limits of Star Formation Discovered by JWST in the COSMOS-Web Survey. , keywords =. doi:10.3847/2041-8213/ad738a , archivePrefix =. 2408.10305 , primaryClass =

    work page doi:10.3847/2041-8213/ad738a 2041

  57. [57]

    , keywords =

    The COSMOS-Web Lens Survey (COWLS) II: Depth, resolution, and NIR coverage from JWST reveals 17 spectacular lenses. , keywords =. doi:10.1093/mnrasl/slaf088 , archivePrefix =. 2503.08782 , primaryClass =

    work page doi:10.1093/mnrasl/slaf088

  58. [58]

    , keywords =

    The COSMOS-Web Lens Survey(COWLS) III: forecasts versus data. , keywords =. doi:10.1093/mnras/staf1678 , archivePrefix =. 2503.08785 , primaryClass =

    work page doi:10.1093/mnras/staf1678

  59. [59]

    , keywords =

    COSMOS-Web: The Role of Galaxy Interactions and Disk Instabilities in Producing Starbursts at z < 4. , keywords =. doi:10.3847/1538-4357/ada566 , archivePrefix =. 2405.09619 , primaryClass =

    work page doi:10.3847/1538-4357/ada566

  60. [60]

    , keywords =

    Resolving Galactic-scale Obscuration of X-Ray AGNs at z 1 with COSMOS-Web. , keywords =. doi:10.3847/2041-8213/acdef4 , archivePrefix =. 2306.03205 , primaryClass =

    work page doi:10.3847/2041-8213/acdef4 2041

  61. [61]

    SCUBADive. I. JWST+ALMA Analysis of 289 Submillimeter Galaxies in COSMOS-web. , keywords =. doi:10.3847/1538-4357/ada357 , archivePrefix =. 2408.08346 , primaryClass =

    work page doi:10.3847/1538-4357/ada357

  62. [62]

    , keywords =

    The COSMOS-Web ring: In-depth characterization of an Einstein ring lensing system at z 2. , keywords =. doi:10.1051/0004-6361/202348095 , archivePrefix =. 2309.15986 , primaryClass =

    work page doi:10.1051/0004-6361/202348095

  63. [63]

    , keywords =

    The COSMOS-Web ring: Spectroscopic confirmation of the background source at z = 5.1. , keywords =. doi:10.1051/0004-6361/202554273 , archivePrefix =. 2502.20136 , primaryClass =

    work page doi:10.1051/0004-6361/202554273

  64. [64]

    , keywords =

    The COSMOS-Web Lens Survey (COWLS) I: discovery of >100 high redshift strong lenses in contiguous JWST imaging. , keywords =. doi:10.1093/mnras/staf1253 , archivePrefix =. 2503.08777 , primaryClass =

    work page doi:10.1093/mnras/staf1253

  65. [65]

    , keywords =

    JWST Discovery of a High-redshift Tidal Disruption Event Candidate in COSMOS-Web. , keywords =. doi:10.3847/1538-4357/adf216 , archivePrefix =. 2504.13248 , primaryClass =

    work page doi:10.3847/1538-4357/adf216

  66. [66]

    , keywords =

    Uncovering a Massive z 7.7 Galaxy Hosting a Heavily Obscured Radio-loud Active Galactic Nucleus Candidate in COSMOS-Web. , keywords =. doi:10.3847/2041-8213/ad11ee , archivePrefix =. 2308.12823 , primaryClass =

    work page doi:10.3847/2041-8213/ad11ee 2041

  67. [67]

    , keywords =

    Two Massive, Compact, and Dust-obscured Candidate z ≃ 8 Galaxies Discovered by JWST. , keywords =. doi:10.3847/1538-4357/acef21 , archivePrefix =. 2304.12347 , primaryClass =

    work page doi:10.3847/1538-4357/acef21

  68. [68]

    , keywords =

    COSMOS-Web: Unraveling the Evolution of Galaxy Size and Related Properties at 2 < z < 10. , keywords =. doi:10.3847/1538-4365/ae0e1b , archivePrefix =. 2504.07185 , primaryClass =

    work page doi:10.3847/1538-4365/ae0e1b

  69. [69]

    , keywords =

    COSMOS-Web: The emergence of the Hubble sequence. , keywords =. doi:10.1051/0004-6361/202553782 , archivePrefix =. 2502.03532 , primaryClass =

    work page doi:10.1051/0004-6361/202553782

  70. [70]

    , keywords =

    The Extended Mapping Obscuration to Reionization with ALMA (Ex-MORA) Survey: 5 Source Catalog and Redshift Distribution. , keywords =. doi:10.3847/1538-4357/ae2fda , archivePrefix =. 2408.14546 , primaryClass =

    work page doi:10.3847/1538-4357/ae2fda

  71. [71]

    Characterisation of SCUBA-2 450um and 850um-selected Galaxies in the COSMOS Field

    Characterization of SCUBA-2 450 m and 850 m selected galaxies in the COSMOS field. , keywords =. doi:10.1093/mnras/stt1673 , archivePrefix =. 1302.2619 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt1673

  72. [72]

    , keywords =

    An Ultradeep Multiband VLA Survey of the Faint Radio Sky (COSMOS-XS): Source Catalog and Number Counts. , keywords =. doi:10.3847/1538-4357/abcaa3 , archivePrefix =. 2009.13528 , primaryClass =

    work page doi:10.3847/1538-4357/abcaa3 2009

  73. [73]

    The VLA-COSMOS 3 GHz Large Project: Continuum data and source catalog release

    The VLA-COSMOS 3 GHz Large Project: Continuum data and source catalog release. , keywords =. doi:10.1051/0004-6361/201628704 , archivePrefix =. 1703.09713 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201628704

  74. [74]

    Euclid preparation. XVII. Cosmic Dawn Survey: Spitzer Space Telescope observations of the Euclid deep fields and calibration fields. , keywords =. doi:10.1051/0004-6361/202142361 , archivePrefix =. 2110.13928 , primaryClass =

    work page doi:10.1051/0004-6361/202142361

  75. [75]

    , keywords =

    Mapping Obscuration to Reionization with ALMA (MORA): 2 mm Efficiently Selects the Highest-redshift Obscured Galaxies. , keywords =. doi:10.3847/1538-4357/ac2eb4 , archivePrefix =. 2110.06930 , primaryClass =

    work page doi:10.3847/1538-4357/ac2eb4

  76. [76]

    COSMOS : Hubble Space Telescope Observations

    COSMOS: Hubble Space Telescope Observations. , keywords =. doi:10.1086/516580 , archivePrefix =. astro-ph/0612306 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/516580

  77. [77]

    , keywords =

    Nature versus Nurture: Revisiting the Environmental Impact on Star Formation Activities of Galaxies. , keywords =. doi:10.3847/1538-4357/ad11d7 , archivePrefix =. 2311.18427 , primaryClass =

    work page doi:10.3847/1538-4357/ad11d7

  78. [78]

    , keywords =

    Large-scale Structures in COSMOS2020: Evolution of Star Formation Activity in Different Environments at 0.4 < z < 4. , keywords =. doi:10.3847/1538-4357/ad32c5 , archivePrefix =. 2312.10222 , primaryClass =

    work page doi:10.3847/1538-4357/ad32c5

  79. [79]

    , author Kartaltepe , J.S

    COSMOS Spectroscopic Redshift Compilation (First Data Release): 488,000 Redshifts Encompassing Two Decades of Spectroscopy. , keywords =. doi:10.3847/1538-4365/ae1cb9 , archivePrefix =. 2503.00120 , primaryClass =

    work page doi:10.3847/1538-4365/ae1cb9

  80. [80]

    , keywords =

    The COSMOS-Web deep galaxy group catalog up to z = 3.7. , keywords =. doi:10.1051/0004-6361/202553759 , archivePrefix =. 2501.09060 , primaryClass =

    work page doi:10.1051/0004-6361/202553759

Showing first 80 references.