REVIEW
The connection between massive galaxies and their dark matter haloes from $z=0.25$ to $z \sim 4$ from the combined COSMOS, XMM-LSS and ECDF-S fields
Astrophysics of Galaxies · Submitted 13 Oct 2026 · 155 references
Pith's verdict: Largest combined deep field analysis to date of the galaxy-halo connection at high mass and high redshift; central claim is plausible but N(z) validation is half-done.
T0 · AI review
Why Pith says this
Highlight any text to comment on it.
Referee report
The paper
The paper claims
Massive galaxies stop growing in stars while their dark-matter haloes keep growing below redshift 1.
The reading
What carries the argument
The five-parameter halo occupation distribution (HOD) model of Zheng et al. (2005), describing central and satellite galaxy occupation as a function of halo mass. The model is fitted to the angular two-point correlation function measured with the Landy–Szalay estimator, using a Markov chain Monte Carlo method that simultaneously fits the number density and clustering in each of three independent survey fields. The redshift distribution N(z) is constructed from photometric-redshift likelihoods with a magnitude-dependent prior and a Gaussian broadening of 0.04(1+z). The model projects the 3D galaxy power spectrum into the angular correlation function via the Limber approximation, allowing the extraction of the stellar-to-halo mass relation and derived quantities such as galaxy bias, satellite fraction, and peak halo/ stellar masses.
Extended reading notes
Core claim
Over the redshift range z=0.25 to z=4, the stellar-to-halo mass ratio for the most massive galaxy population peaks at z~1. Below z=1, the peak halo mass M_h^peak increases (from ~$10^{12}$.5 to ~$10^{13}$ M_sun in the highest stellar-mass bin), while the peak stellar mass M_*^peak in those haloes remains approximately constant at ~5×$10^{10}$ M_sun. This divergence implies that from z=1 to today, massive haloes grow through hierarchical accretion but their central galaxies do not build up additional stars. The satellite fraction also rises steadily since z~1, consistent with haloes growing via accretion of smaller systems whose central galaxies become satellites. The combined evidence points to a mechanism that suppresses star formation in the most massive central galaxies at late times, and the authors attribute this to radio-mode AGN feedback.
Load-bearing premise
The redshift distribution N(z) of each galaxy sample, constructed from photometric-redshift likelihoods with a magnitude-dependent prior and a Gaussian broadening of width 0.04(1+z), is assumed to be accurate; the authors acknowledge that misrepresentations in the shape of N(z), especially its wings, can cause up to 20–50% differences in the predicted angular correlation function, and that at z>1.5 the HOD parameter sigma_logM hits its upper prior boundary, indicating that the N(z) uncertainty is not fully resolved.
Editorial extensions
If this is right
- If true, the suppression of stellar-mass growth in massive haloes below z~1 implies that AGN feedback is the primary quenching mechanism for the most massive galaxies in the nearby Universe, consistent with semi-analytic models that couple radio-jet heating to the hot gas halo.
- The increasing satellite fraction with decreasing redshift suggests that halo mass assembly at z<1 occurs primarily through the accretion of pre-formed galaxies rather than through in-situ star formation in the central galaxy.
- The redshift z~1 marks the epoch at which the star-formation efficiency in massive haloes peaks; above z=1 the efficiency declines because haloes are still assembling rapidly, and below z=1 it declines because star formation shuts off.
- The finding motivates targeted radio observations of massive galaxies at z<1 to quantify the duty cycle of low-power radio jets and their correlation with the star-formation history of the central galaxy.
Reading between the lines
- The result provides an observational anchor for galaxy-formation simulations: any model that fails to reproduce the decoupling of stellar-mass and halo-mass growth at z<1 may be missing a key feedback process or overestimating the late-time gas accretion rate.
- If the suppression is indeed due to AGN feedback, one expects that the most massive central galaxies at z<0.5 should host compact radio cores or show evidence of recent mechanical feedback in X-ray cavities; upcoming surveys with MeerKAT and the SKA can test this directly.
- The combined-field approach reduces cosmic variance by a factor ~2 compared to single-field studies; future surveys such as Euclid and Rubin will be able to extend this analysis to even larger volumes and fainter stellar-mass thresholds, testing whether the effect holds for lower-mass galaxies as well.
Original abstract
Understanding how galaxies populate and grow within dark matter haloes is essential for linking the observed evolution of galaxies to the hierarchical growth of structure. We present a galaxy clustering analysis using optical and near-infrared data from the UltraVISTA and VIDEO surveys covering $9.3$ deg$^2$ across the COSMOS, XMM-LSS and ECDF-S fields, $\sim 5\times$ larger than previous comparable studies, providing sufficient volume to determine the halo occupation of the most massive galaxies to $z\sim 4$. We measure the angular two-point correlation function for stellar-mass-selected galaxies over $0.25<z<4$ and by combining the three fields, we reduce the cosmic variance by a factor of $\sim2$ compared to the individual fields. The stellar-to-halo mass ratio peaks at a halo mass of $M_{h}\approx10^{12} {\rm M}_{\odot}$ and is a maximum at $z\sim 1$. For the most massive galaxies, the peak halo mass ($M_{h}^{\rm peak}$) increases from $z=1\rightarrow 0$, while the peak stellar mass in such haloes remains approximately constant, indicating that at $z<1$ massive galaxy formation becomes less efficient. We also find a steady increase in the satellite fraction since $z\sim 1$, from which we infer that massive halos continue to grow hierarchically while their central galaxies experience suppressed stellar-mass growth. We suggest this is due to the central massive galaxies having their growth controlled by feedback from active galactic nuclei feedback, likely from low-power stochastic radio emission.
The compiled record
The paper's own sentences, arranged, kept beside the review and separate from it. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
The abstract, sentence by sentence
Understanding how galaxies populate and grow within dark matter haloes is essential for linking the observed evolution of galaxies to the hierarchical growth of structure. We present a galaxy clustering analysis using optical and near-infrared data from the UltraVISTA and VIDEO surveys covering $9.3$ deg$^2$ across the COSMOS, XMM-LSS and ECDF-S fields, $\sim 5\times$ larger than previous comparable studies, providing sufficient volume to determine the halo occupation of the most massive galaxies to $z\sim 4$. We measure the angular two-point correlation function for stellar-mass-selected galaxies over $0.25<z<4$ and by combining the three fields, we reduce the cosmic variance by a factor of $\sim2$ compared to the individual fields. The stellar-to-halo mass ratio peaks at a halo mass of $M_{h}\approx10^{12} {\rm M}_{\odot}$ and is a maximum at $z\sim 1$. For the most massive galaxies, the peak halo mass ($M_{h}^{\rm peak}$) increases from $z=1\rightarrow 0$, while the peak stellar mass in such haloes remains approximately constant, indicating that at $z<1$ massive galaxy formation becomes less efficient. We also find a steady increase in the satellite fraction since $z\sim 1$, from which we infer that massive halos continue to grow hierarchically while their central galaxies experience suppressed stellar-mass growth. We suggest this is due to the central massive galaxies having their growth controlled by feedback from active galactic nuclei feedback, likely from low-power stochastic radio emission.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Understanding how galaxies populate and grow within dark matter haloes is essential for linking the observed evolution of galaxies to the hierarchical growth of structure. | background 1.00 | 0.04 | 0.03 | asserted 1.00 |
| s1 | We present a galaxy clustering analysis using optical and near-infrared data from the UltraVISTA and VIDEO surveys covering $9.3$ deg$^2$ across the COSMOS, XMM-LSS and ECDF-S fields, $\sim 5\times$ larger than previous comparable studies, providing sufficient volume to determine the halo occupation of the most massive galaxies to $z\sim 4$. | contribution 0.54 | 0.96 | 0.04 | asserted 1.00 |
| s2 | We measure the angular two-point correlation function for stellar-mass-selected galaxies over $0.25<z<4$ and by combining the three fields, we reduce the cosmic variance by a factor of $\sim2$ compared to the individual fields. | method 0.89 | 0.98 | 0.04 | asserted 1.00 |
| s3 | The stellar-to-halo mass ratio peaks at a halo mass of $M_{h}\approx10^{12} {\rm M}_{\odot}$ and is a maximum at $z\sim 1$. | result 1.00 | 0.92 | 0.24 | asserted 1.00 |
| s4 | For the most massive galaxies, the peak halo mass ($M_{h}^{\rm peak}$) increases from $z=1\rightarrow 0$, while the peak stellar mass in such haloes remains approximately constant, indicating that at $z<1$ massive galaxy formation becomes less efficient. | result 0.90 | 0.92 | 0.31 | asserted 0.58 |
| s5 | We also find a steady increase in the satellite fraction since $z\sim 1$, from which we infer that massive halos continue to grow hierarchically while their central galaxies experience suppressed stellar-mass growth. | result 0.54 | 0.97 | 0.21 | asserted 0.98 |
| s6 | We suggest this is due to the central massive galaxies having their growth controlled by feedback from active galactic nuclei feedback, likely from low-power stochastic radio emission. | interpretation 1.00 | 0.56 | 0.18 | hedged possibility 0.98 |
What was examined, and what was not
- arXiv listing abstract v1
- full text
- figures and tables
- references and citing sentences
- relations to other papers
- P abstract
- S sections
- T body sentences
- C citations
- R cross-paper relations
Figures
Figures reproduced from arXiv:2610.19030 by the authors.
References
Discussion
Disagree with the review, or know something it missed? Leave a comment, highlight any passage above to comment on it, or challenge this review formally.