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REVIEW 3 major objections 5 minor 170 references

The influence of feedback on the baryonic content of haloes in the COLIBRE simulations

T0 review · 3 major / 5 minor · reviewed 2026-08-01 · deepseek-v4-flash

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Pith's one-line read Halo gas fractions are a sensitive probe of feedback: COLIBRE and its predecessor produce similar galaxies but very different gas contents in groups and clusters, and the difference traces to a black-hole-mass-scaled AGN heating temperature

desk verdict Solid, transparent simulation paper with genuinely new COLIBRE gas-fraction predictions, but the abstract oversells the resolution/dataset dependence of the 'better agreement' claim. read the letter →

arxiv 2607.27319 v1 pith:JQ2L3ZY2 submitted 2026-07-29 astro-ph.GA

Jonathan J. Davies (1) , Joop Schaye (2) , Filip Huško (2) , Ruby J. Wright (3) , Evgenii Chaikin (4 , 2) , Matthieu Schaller (2) , Robert J. McGibbon (2)
show 22 more authors
Alejandro Benítez-Llambay (5) Sylvia Ploeckinger (6) Alexander J. Richings (7 8) ((1) Astrophysics Research Institute Liverpool John Moores University (2) Leiden Observatory Leiden University (3) International Centre for Radio Astronomy Research University of Western Australia (4) Institute for Computational Cosmology Department of Physics University of Durham (5) Dipartimento di Fisica "Giuseppe Occhialini'' Università degli Studi di Milano-Bicocca (6) Department of Astrophysics University of Vienna (7) Centre for Data Science Artificial Intelligence Modelling University of Hull (8) E. A. Milne Centre for Astrophysics University of Hull)
This is my paper
classification astro-ph.GA
keywords halogasfractionsAGNfeedbacksupernovacosmologicalsimulationsgalaxygroupsandclusterscircumgalacticmediumkineticSunyaev-Zel'dovicheffecteROSITA
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper uses the COLIBRE suite of cosmological simulations to establish how feedback from supernovae and active galactic nuclei sets the gas content of dark-matter haloes, from dwarf galaxies to galaxy clusters. Its central result is that the halo gas fraction versus halo mass relation is a far more discriminating test of feedback physics than the galaxy population alone: COLIBRE and its predecessor EAGLE reproduce similar galaxies, yet COLIBRE keeps substantially less gas in group- and cluster-scale haloes, agreeing better with X-ray and kinetic Sunyaev-Zel'dovich measurements. The paper traces this improvement to a single design choice, scaling the AGN heating temperature linearly with black hole mass, so feedback events become more energetic precisely where they must overcome deep potential wells. A second, more realistic 'hybrid' AGN model that adds jets lowers group gas fractions further, matching the newest eROSITA stacks and kSZ constraints without degrading the agreement with galaxy observations. If this is right, measuring the gas content of haloes, not just the galaxies inside them, can break the degeneracy between feedback models that currently pass the same galaxy tests.

What carries the argument

The load-bearing object is the AGN heating temperature increment ΔT_AGN, which scales with black hole mass, so the energy per feedback event grows with it. This scaling lets AGN feedback expel gas from the deep potential wells of groups and clusters, where a fixed heating increment fails. The hybrid model applies the same idea through a jet velocity scaling with the square root of black hole mass, half the energy traveling in collimated jets that couple to gas efficiently. A second mechanism, a supernova heating temperature scaling with gas density, makes stellar feedback gentler and raises gas fractions in dwarf haloes. These scalings drive the non-monotonic f_gas-M relation and COLIBRE's l

What would settle it

The cleanest check is a single-change simulation: take the fiducial model at fixed resolution and replace the BH-mass-scaled ΔT_AGN with a fixed value (the predecessor's 10^8.5 K) without re-calibrating anything; if group gas fractions do not rise back toward the predecessor's values, the scaling is not the cause. Observationally, the available group gas fractions are mutually inconsistent: a cross-calibration of eROSITA stacks, XMM-Newton profiles, and kSZ baryonification constraints at M500 ~ 10^13-10^14 M_sun that converged on one value would decide whether the low fractions the hybrid mode

Watch

Extended reading notes

Core claim

COLIBRE's claim: halo gas fractions are non-monotonic in halo mass, peaking near 10^11.5-12 M_sun; supernova feedback strips dwarf haloes, AGN feedback depletes groups and clusters. The fiducial thermal model, whose heating increment ΔT_AGN scales with black hole mass, matches Chandra/XMM-Newton gas fractions but runs high versus eROSITA stacks and kSZ-derived values; the hybrid thermal-plus-jet model runs lower and matches those newer data. The paper attributes the reduction mostly to the BH-mass scaling, which makes feedback events more energetic where potential wells are deepest; most expulsion occurs above the predecessor's fixed 10^8.5 K heating. Both variants were calibrated to observe

Load-bearing premise

The claim that black-hole-mass-scaled AGN heating is what makes COLIBRE's groups and clusters gas-poor rests on model variants that removed that feature while also re-calibrating other parameters, so the scaling itself, rather than a correlated choice such as black hole seed mass or coupling efficiency, is the assumed cause—and separately, gas fractions rise with resolution, so the observed-level comparison is not unique.

Editorial extensions

If this is right

  • Simulations whose AGN heating does not grow with black hole mass will tend to over-predict the gas content of groups and clusters, and hence under-predict the feedback-driven suppression of the matter power spectrum on group scales; Appendix D shows COLIBRE expels most baryons with a heating temperature well above the predecessor's fixed value.
  • Galaxy-scale observables alone cannot fix the baryon content of haloes: two calibrated COLIBRE variants pass the same galaxy tests yet differ significantly in halo gas, a degeneracy the paper argues only halo-gas observations can break.
  • The hybrid jet model reaches the low group gas fractions suggested by eROSITA and kSZ data within a model that still matches galaxy populations, showing the stronger feedback those data appear to require is compatible with a successful galaxy formation model (with the paper's caveat that comparably strong models can fail like-for-like X-ray comparisons of cluster thermodynamics).
  • Gas fractions increase with resolution at fixed halo mass in COLIBRE, so the same physics gives different observed-level gas fractions at different resolutions; any simulation-observation comparison must be read at a specified resolution.
  • The expulsion-then-re-accretion sequence — clusters re-accrete gas and end up gas-rich while groups stay depleted — explains how strong-feedback models can lower group gas fractions without over-depleting clusters, because cluster progenitors were depleted less and replenish later.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • A controlled experiment the paper does not run: replace ΔT_AGN with a fixed value inside the fiducial model without re-calibrating anything, and re-measure group-scale gas fractions; the paper's re-calibrated variants leave the scaling entangled with other parameter changes, so this single-change test would isolate the cause.
  • The resolution trend means inferred feedback strength from kSZ and X-ray 'missing baryons' analyses is likely resolution-degenerate in the same direction: higher-resolution runs of one model bracket observations differently, so observational claims of strong feedback should be quoted against a specific resolution.
  • COLIBRE's cold-gas census — up to half of halo gas below 10^4.5 K at M200 near 10^11.4 M_sun, down to 10 K — is invisible to the X-ray and kSZ constraints this paper compares against; CGM absorption-line surveys of low-mass haloes could test that temperature breakdown directly.
  • The lower group gas fractions imply stronger baryon-feedback suppression of the matter power spectrum on group scales than the predecessor predicted; plugging COLIBRE's f_gas relation into baryonification fits to kSZ data is a direct way to test whether a COLIBRE-like baryon model also addresses the current S8 tension.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 5 minor

Summary. The paper presents predictions for the z=0 halo gas mass fraction relation f_gas-M_200 in the COLIBRE cosmological simulations, using three resolution levels and two AGN feedback prescriptions (fiducial thermal and hybrid thermal/jet). It reports a non-monotonic relation, a multiphase census of halo gas, and significant resolution dependence. Comparisons with X-ray and kSZ constraints show that the m6 fiducial model matches pre-eROSITA X-ray data while the m7 hybrid model matches eROSITA and kSZ constraints. The paper argues that COLIBRE generally produces lower group/cluster gas fractions than EAGLE and most contemporary simulations, attributes this mainly to the BH-mass-dependent AGN heating temperature ΔT_AGN (and, in the hybrid model, to jets), and explores the redshift history of gas expulsion and re-accretion.

Significance. The strength of the paper is that COLIBRE was calibrated to galaxy stellar mass functions and size-mass relations, not to halo gas fractions, so the f_gas-M_200 relation is a genuine prediction. The use of multiple resolutions and two calibrated AGN prescriptions, plus the comparison with a broad set of observational constraints, makes this a valuable contribution. The demonstration that two models with similar galaxy populations can have substantially different halo gas content is an important result for feedback modelling. The paper is also transparent about the non-convergence with resolution and the inconsistency between observational datasets. If the claims are appropriately qualified, this will be a useful reference for interpreting eROSITA and kSZ constraints.

major comments (3)
  1. [Abstract; §3.1.2, Fig. 3] The headline claim that "COLIBRE produces lower gas fractions for groups and clusters than EAGLE and other contemporary simulations, and better agreement with observational constraints" is not a single, resolution-independent claim. §3.1.2 and Fig. 1 show that f_gas at fixed M_200 increases with resolution and is not converged. In Fig. 3, the m6 fiducial simulation agrees with the pre-eROSITA X-ray compilation but is high relative to eROSITA/kSZ constraints, while the m7 simulation falls below the pre-eROSITA data. In Fig. 4, the m7 hybrid model matches eROSITA/kSZ but is low relative to pre-eROSITA data. Since §3.2.3 states that the observational constraints are mutually inconsistent, "better agreement" is conditional on choosing one resolution and one dataset. The body is transparent about this, but the abstract and the summary bullets present the result as robust and unique. Please qu
  2. [§3.4.1, Appendix C/D] The causal attribution of COLIBRE's lower group/cluster gas fractions relative to EAGLE to the BH-mass-dependent ΔT_AGN (Eq. 7) is only partially supported. The model variants in Appendix C were each independently recalibrated, and the paper itself states that "the removal of individual model features ... are therefore not strictly the only changes made." The non-calibrated AGN parameter variations in Fig. C1 do show that ΔT_AGN affects f_gas, and Appendix D shows that in L200m6 the bulk of AGN-driven expulsion occurs at ΔT_AGN higher than EAGLE's fixed 10^8.5 K. However, other BH modelling changes (repositioning, super-Eddington accretion, changed energy injection method) are acknowledged as potential contributors. The conclusion that the improvement "can be attributed to" the ΔT_AGN scaling is therefore stronger than the evidence. Please soften to "is consistent with" or, ideally, add
  3. [§3.3, Fig. 4] The comparison between the fiducial and hybrid AGN models is not a controlled experiment: the hybrid simulations also use different calibrated values of the BH seed mass and feedback efficiencies, and §3.3 states that the seed-mass difference amplifies the m7 difference. Thus the statement "the hybrid AGN feedback model produces lower gas fractions" describes the effect of the whole recalibrated model variant, not of the jet prescription alone. This distinction matters for the abstract's claim that a "hybrid AGN feedback model" produces lower gas fractions. Either present these as model-level comparisons, or add a run in which only the jet/wind mechanism is changed while all other calibration parameters are held fixed.
minor comments (5)
  1. [Fig. 2 / Fig. A1] The stacked temperature-bin bars in Fig. 2 and Fig. A1 are informative, but the stacking order is not stated. A sentence in the caption explaining the order (e.g. coldest at bottom) would help.
  2. [Fig. 3] The grey shaded bands from the two baryonification models are easily confused with individual data points. Consider using labelled filled bands with distinct edge styles.
  3. [§2.4] The definition of f_gas includes all gas within r_500, while the X-ray/kSZ constraints largely trace hot gas. The temperature-cut comparison is given later, but a one-sentence reminder in the Fig. 3/4 captions would improve readability.
  4. [§3.2.1] Typo: "observational contraints" should be "observational constraints."
  5. [Appendix C] The model variant names (ThermalKinetic_varΔT_SN_varfE etc.) are hard to parse. A small table or a list with the deactivated features would make the comparison much easier to follow.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the fgas predictions are not calibrated inputs and the key attributions are tested by controlled model variants.

full rationale

The paper's central claim is that COLIBRE's fgas-M200 relation is a prediction of a model calibrated to galaxy stellar masses and sizes, not to halo gas fractions. The paper states explicitly: 'the subgrid prescriptions in COLIBRE and the parameter values used in those prescriptions were not calibrated at any resolution to reproduce observed constraints on halo gas fractions' (Section 3.1.2). The comparison with X-ray, eROSITA, and kSZ data is therefore a genuine out-of-sample test, not a fitted parameter renamed as a prediction. The attribution of COLIBRE's lower group/cluster gas fractions to the BH-mass-dependent AGN heating temperature (Eq. 7) is supported by controlled, non-calibrated variants in Appendix C (right panel of Fig. C1) in which only DeltaT_AGN or epsilon_f is varied, and by the redshift evolution of DeltaT_AGN in Appendix D. The left panel of Fig. C1 does use individually recalibrated variants from Chaikin et al. (2026b), and the paper honestly notes that 'the removal of individual model features ... are therefore not strictly the only changes made'; this is a limitation on isolating individual feedback components, but it is not circular because the recalibration targets are galaxy population observables, not fgas. Self-citations to Schaye et al. (2026), Chaikin et al. (2026b), and Huško et al. (2026) define the simulation model and its calibration, which is standard practice; they do not supply the fgas values or the agreement with observations, which are computed and compared here for the first time. No self-definitional loop, no uniqueness theorem imported from the authors, and no ansatz smuggled in via citation were found. The resolution and dataset dependence of the observational comparison is a scientific caveat, not circularity.

Assumptions & free parameters 7 free parameters · 4 assumptions · 0 invented entities

The central predictions rest on the calibrated COLIBRE subgrid model rather than on first principles; no new physical entities are introduced. The free parameters listed are calibrated to galaxy-scale observables, not to halo gas fractions, which keeps the fgas comparison partly predictive.

free parameters (7)
  • f_E,min (minimum CCSN energy per supernova) = 0.1–0.8 (calibrated per resolution)
    Sets minimum energy of stochastic thermal SN feedback; controls low-mass halo gas expulsion.
  • P_E,pivot (pressure pivot for f_E) = 8.0e3–1.5e4 K cm^-3
    Determines pressure dependence of SN energy; calibrated to match GSMF and sizes.
  • n_H,pivot (density pivot for ΔT_SN) = 0.5–1.5 cm^-3
    Controls density-dependent SN heating temperature; affects how expulsive SN feedback is in low-density gas.
  • ΔT_AGN,max (maximum AGN heating temperature) = 10^9.5 K (m7), 10^10 K (m6/m5)
    Caps energy per AGN feedback event; directly affects group/cluster gas fractions.
  • ε_f (AGN feedback coupling efficiency) = 0.1 (m7), 0.05 (m6/m5)
    Sets AGN energy coupling; affects BH self-regulation and hence fgas via BH mass.
  • m_BH,seed (SMBH seed mass) = 2e4–5e5 M_sun
    Influences onset and efficiency of AGN feedback, especially in low-mass haloes and at m7 resolution.
  • Hybrid AGN jet/wind efficiencies (ε_jet, ε_wind, ε_accr)
    Set by subgrid disc state model (Huško+26); not detailed here but affect jet feedback strength and lower fgas.
assumptions (4)
  • domain assumption DES Y3 ΛCDM cosmology (Ω_M=0.306, Ω_b=0.0486, σ8=0.807, h=0.681, n_s=0.967, m_ν=0.06 eV) is the correct background cosmology.
    Used for initial conditions in §2; not derived.
  • domain assumption Subgrid prescriptions for unresolved processes (cooling/chemistry, star formation, SN/AGN feedback) are adequate representations of the real physics that sets halo gas fractions.
    The whole analysis depends on these models (Schaye+26; Chaikin+26b), which are not first-principles.
  • domain assumption The SPHENIX SPH scheme and Swift code accurately capture hydrodynamics at resolved scales, including multiphase gas, outflows, and halo gas retention.
    References §2, Borrow+22, Schaller+24; numerical choices could affect fgas.
  • domain assumption HBT-HERONS and SOAP correctly identify central haloes/subhaloes and define M_200/M_500 and gas fractions.
    §2.4; halo definition choices can affect comparisons.

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Cite this review

Pith. "Pith review of The influence of feedback on the baryonic content of haloes in the COLIBRE simulations." pith.science (2026). https://pith.science/paper/JQ2L3ZY2

@misc{pith2026260727319,
  author       = {Pith},
  title        = {Pith review of: The influence of feedback on the baryonic content of haloes in the COLIBRE simulations},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/JQ2L3ZY2}},
  note         = {Machine review of arXiv:2607.27319}
}
abstract

We present predictions for the relation between the halo gas mass fraction and halo mass, $f_{\rm gas}^{200}-M_{200}$, from the COLIBRE cosmological simulations of galaxy formation, and explore how the gas content of haloes is influenced by feedback from supernovae and active galactic nuclei (AGN) over time. The $f_{\rm gas}^{200}-M_{200}$ relation in COLIBRE is non-monotonic, with a peak at $M_{200}\sim 10^{11.5-12}$~M$_\odot$. Below this mass, feedback from supernovae efficiently expels gas from the haloes of dwarf galaxies, and above it, AGN feedback efficiently depletes the haloes of galaxy groups. The fiducial COLIBRE model yields gas fractions for galaxy groups and clusters that agree with constraints from Chandra and XMM-Newton X-ray data, but which are high relative to gas fractions inferred from eROSITA stacks and measurements of the kinetic Sunyaev-Zel-dovich (kSZ) effect. COLIBRE's hybrid AGN feedback model, which combines thermal and jet-driven feedback, produces lower gas fractions in better agreement with eROSITA and kSZ measurements. COLIBRE produces lower gas fractions for groups and clusters than EAGLE and other contemporary simulations, and better agreement with observational constraints. We investigate the origin of this improvement relative to EAGLE, and how the resolution of the simulation affects the impact of feedback. Our results demonstrate that halo gas fractions are a sensitive probe of feedback physics, and that they can differ significantly between simulations that otherwise produce very similar galaxy populations.

Figures

Figures reproduced from arXiv: 2607.27319 by the authors.

Figure 1
Figure 1. Halo baryon fractions ( 𝑓 200 b , upper panel), stellar fractions ( 𝑓 200 ★ , middle panel) and gas mass fractions ( 𝑓 200 gas , lower panel), within radius 𝑟200, as a fraction of halo mass 𝑀200, for the L400m7, L200m6 and L025m5 COLIBRE simulations at 𝑧 = 0. All fractions are normalised to the cosmic baryon fraction, 𝑓 cosmic b = Ωb/ΩM. Solid lines show the median relation in bins of halo mass, and shading shows th… view at source ↗
Figure 2
Figure 2. Left panel: the distribution of temperatures, 𝑇, and hydrogen number densities, 𝑛H, for gas particles bound to haloes with 𝑀200 > 1011 M⊙ in the L200m6 simulation at 𝑧 = 0. The coloured regions highlighted along the temperature axis indicate the bins used in the right-hand panel, which shows the contribution of gas within these temperature bins to the mean 𝑓 200 b − 𝑀200 relation, in addition to the contribution fro… view at source ↗
Figure 3
Figure 3. The present-day 𝑓 500 gas − 𝑀500 relation in the L400m7 and L200m6 simulations, compared with observational constraints. Data points show pre￾eROSITA X-ray data compiled by Kugel et al. (2023), including their two data points derived from Akino et al. (2022), and the results of eROSITA stacking analyses by Zhang et al. (2026), Popesso et al. (2026) and Lyskova et al. (2023), plus data from low-redshift X-ray detecte… view at source ↗
Figures from the paper (4 more)
Figure 4
Figure 4. Figure 4: Influence of the AGN feedback prescription on the present-day 𝑓 500 gas − 𝑀500 relation in COLIBRE, at m6 (left panel) and m7 (right panel) resolution levels. We compare the fiducial L200m6 and L400m7 simulations, run with purely thermally-driven AGN feedback, to the l…
Figure 5
Figure 5. Figure 5: The present-day 𝑓 500 gas − 𝑀500 relation in COLIBRE, compared with the predictions of other contemporary simulations with similar mass resolution. The left-hand panel shows simulations with baryonic particle mass 𝑚b ∼ 106 M⊙: COLIBRE L200m6, EAGLE L100m6 (RefL100N1504…
Figure 6
Figure 6. Figure 6: Evolution of the COLIBRE 𝑓 200 gas − 𝑀200 relation from 𝑧 = 4 to the present day, at m6 (upper panel) and m7 (lower panel) resolution, in the fiducial model (thick lines) and hybrid AGN model (thin lines). Dotted lines indicate low-mass bins containing poorly-resolved …
Figure 7
Figure 7. Figure 7: Evolution of 𝑓 200 gas with redshift for haloes binned by present-day halo mass, 𝑀𝑧=0 200 , at both m6 and m7 resolutions, and with both thermal and hybrid AGN feedback. Solid lines show the median 𝑓 200 gas , and dotted lines indicate where the median stellar mass is …

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Pith tools

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