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arxiv: 2606.10028 · v1 · pith:COXTZ5AInew · submitted 2026-06-08 · 🌌 astro-ph.CO · astro-ph.GA

Learning the Universe: Constrained simulations of the Coma galaxy cluster -- I. Radial X-ray and Compton-y signatures

Ulrich P. Steinwandel , Stuart McAlpine , Richard Stiskalek , R\"udiger Pakmor , Volker Springel , Eugene Churazov , Ildar Khabibullin , Jens Jasche
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Guilhem Lavaux Greg L. Bryan
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Pith reviewed 2026-06-27 15:14 UTC · model grok-4.3

classification 🌌 astro-ph.CO astro-ph.GA
keywords constrained simulationsComa clusterX-ray surface brightnessSunyaev-Zel'dovich effectintracluster mediumgalaxy formation modelcosmological simulationscluster analogues
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The pith

Constrained simulations of Coma analogues reproduce the broad shape and normalisation of observed X-ray and Compton-y profiles.

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

The paper presents a suite of 50 simulations that select regions from BORG/MANTICORE constrained initial conditions expected to form massive clusters like Coma and evolve them with the IllustrisTNG model. These runs generate realistic galaxy populations and intracluster medium properties that are then compared directly to eROSITA X-ray surface brightness profiles and Planck thermal Sunyaev-Zel'dovich Compton-y measurements. The work shows that the simulated profiles match the observed shape and amplitude while also mapping out the scatter attributable to differences in environment and assembly history. A reader would care because the approach supplies a statistically controlled way to place a specific observed cluster inside a full cosmological context rather than treating it in isolation.

Core claim

The ensemble of 50 high-fidelity Coma analogues reproduces the broad shape and normalisation of both the X-ray surface brightness profiles extracted from the simulations and the integrated Compton-y profiles, while quantifying the range of scatter expected from environmental and assembly-history variations. This match holds across the selected regions that form clusters comparable to Coma in mass and environment. The resulting dataset therefore supplies a controlled laboratory for assessing how feedback, mergers, and large-scale environment shape observable intracluster medium properties.

What carries the argument

The BORG/MANTICORE constrained initial conditions that identify regions forming Coma-like clusters, evolved forward with the IllustrisTNG galaxy formation model to produce the intracluster medium whose X-ray and thermal Sunyaev-Zel'dovich signatures are extracted.

If this is right

  • The simulations enable direct assessment of how feedback processes and merger activity influence observable cluster properties.
  • The ensemble supplies a statistically robust framework for interpreting Coma within its cosmological context that accounts for cosmic variance.
  • The dataset can be used to test models of intracluster medium physics and to calibrate scaling relations for nearby massive clusters.
  • The same strategy of constrained initial conditions plus state-of-the-art galaxy formation physics can generate targeted analogues for other observed clusters.

Where Pith is reading between the lines

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

  • The method could be extended to build ensembles for additional nearby clusters, allowing statistical comparison of assembly histories across the local volume.
  • The quantified scatter from environment may help reconcile apparent tensions between different cluster observables when samples are drawn from varying large-scale environments.
  • Joint X-ray and Sunyaev-Zel'dovich analyses of future observations could be interpreted against this simulation library to tighten constraints on feedback efficiency.

Load-bearing premise

The constrained initial conditions correctly pick out regions that form clusters matching Coma in mass and environment, and the IllustrisTNG model adequately captures the intracluster medium physics needed for the X-ray and Compton-y comparisons.

What would settle it

If the full set of 50 simulated X-ray surface brightness profiles or Compton-y profiles lies systematically outside the observed eROSITA or Planck data by more than the reported scatter range, the reproduction claim would be falsified.

Figures

Figures reproduced from arXiv: 2606.10028 by Eugene Churazov, Greg L. Bryan, Guilhem Lavaux, Ildar Khabibullin, Jens Jasche, Richard Stiskalek, R\"udiger Pakmor, Stuart McAlpine, Ulrich P. Steinwandel, Volker Springel.

Figure 1
Figure 1. Figure 1: Coma_025 constrained overview. The big top panel shows the gas surface density with in-plane velocity streamlines, the BCG stellar-light zoom-in, and the radial Compton-𝑦 and X-ray surface brightness profiles; the middle row compares the observed Planck and SRG/eROSITA maps to the simulation, and the bottom row shows the dark matter, metallicity, magnetic field, and stellar surface density. All panels are … view at source ↗
Figure 2
Figure 2. Figure 2: Projected dark-matter surface density maps for all 50 constrained Coma analogues (labelled Coma_000 to Coma_049), arranged in a 5 × 10 grid. Each panel spans a 10 × 10 Mpc field of view centred on the Coma analogue. The projection is computed by ray-tracing the Voronoi cell geometry along the 𝑧-axis. White dashed and solid circles indicate 𝑅500𝑐 and 𝑅200𝑚, respectively. The uniform logarithmic colour scale… view at source ↗
Figure 3
Figure 3. Figure 3: Projected gas surface density maps for all 50 constrained Coma analogues, in the same 5 × 10 layout as [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Hot gas fraction 𝑓gas = 𝑀gas(< 𝑅500𝑐 ) / 𝑀500𝑐 as a function of total halo mass 𝑀500𝑐 for the 50 constrained Coma analogues. The simulated clusters are compared with observational estimates from the X-ray group and cluster samples of Giodini et al. (2009), Gonzalez et al. (2013), Lovisari et al. (2015), Lovisari et al. (2020), and the kSZ stacking analysis of Tanimura et al. (2021). All masses and gas frac… view at source ↗
Figure 5
Figure 5. Figure 5: Integrated thermal Sunyaev–Zel’dovich signal 𝑌SZ,500 (top) and soft X-ray luminosity 𝐿𝑋 in the 0.5–2 keV band (bottom) as a function of 𝑀500𝑐 for the 50 constrained Coma analogues. Top: observational relations from Planck Collaboration et al. (2014), and the central-bias-corrected Hill et al. (2018) model, along with points from Nagarajan et al. (2019) and Adam et al. (2024). Self-similar 𝑌 ∝ 𝑀5/3 is indic… view at source ↗
Figure 6
Figure 6. Figure 6: Soft X-ray luminosity 𝐿𝑋 (0.5–2 keV) versus BCG stellar mass 𝑀★,BCG (< 30 kpc) for all 50 constrained Coma analogues, compared with the ROSAT stacking results of Anderson et al. (2015) and their best-fit power law (𝛼 = 3.34). Our simulated clusters occupy the high-stellar-mass end of this relation and are consistent with the Anderson et al. (2015) trend extrapolated to cluster-BCG scales. the constrained e… view at source ↗
Figure 7
Figure 7. Figure 7: Supermassive black hole scaling relations for the BCG in each of the 50 constrained Coma analogues. Left: 𝑀BH versus 𝑀500𝑐, compared with the dynamical measurements of Bogdán et al. (2018), the Gaspari et al. (2019) sample (tables converted 𝑇𝑋,𝑐 to 𝑀500𝑐 via Lovisari et al. 2015), and the Bassini et al. (2019) Dianoga best-fit relation with 1𝜎 scatter band. Right: 𝑀BH versus the 1D stellar velocity dispers… view at source ↗
Figure 8
Figure 8. Figure 8: Stellar mass scaling relations for the 50 constrained Coma analogues. Left: BCG stellar mass 𝑀★,BCG (< 30 kpc) vs 𝑀500𝑐, compared with the individual-cluster measurements and best-fit relation of Kravtsov et al. (2018), the BCG relation of Akino et al. (2022), and the central-galaxy SHMR curves from Behroozi et al. (2019), Moster et al. (2018), and Leauthaud et al. (2012). Halo-mass definitions from abunda… view at source ↗
Figure 9
Figure 9. Figure 9: Projected radial surface number density profiles Σgal(𝑟 ) of satellite galaxies around the Coma analogue in each of the 50 realisations, for three stellar mass thresholds (𝑀★ > 109 , 1010, and 1010.5 M⊙). Solid lines show the mean across all realisations; shaded bands indicate 16–84th percentile scatter. Black circles show Budzynski et al. (2012) (SDSS, log 𝑀500 = 14.7– 15.0, 𝑀𝑟 ≤ −20.5). A power-law refer… view at source ↗
Figure 10
Figure 10. Figure 10: Projected maps of the ICM for 8 representative realisations (Coma_000–Coma_007), each panel a 10 × 10 Mpc field of view along the 𝑧-axis. Top row: Compton-𝑦 = (𝜎T/𝑚𝑒𝑐 2 ) ∫ 𝑛𝑒 𝑘B𝑇 d𝑙, log scale 10−8–10−4 . Bottom row: X-ray surface brightness (0.4–2 keV) from APEC cooling tables (Smith et al. 2001; Foster et al. 2012) using per-particle 𝑋H, 𝑛𝑒, 𝑇; log scale 10−10–10−4 erg s−1 cm−2 . in a two-panel layout.… view at source ↗
Figure 11
Figure 11. Figure 11: Azimuthally averaged radial profiles for all 50 constrained Coma analogues (green lines). Left: Compton-𝑦 vs 𝑟/𝑅500𝑐, compared with Planck Collaboration et al. (2013, grey pentagons) and the MillenniumTNG prediction of Pakmor et al. (2023, solid red). Right: X-ray surface brightness (0.5–2 keV) vs angular radius (assuming 𝑅200𝑐 ≈ 70 arcmin for Coma), compared with SRG/eROSITA observations of Churazov et a… view at source ↗
Figure 12
Figure 12. Figure 12: Radial profiles of the 10 best-fitting realisations, selected by minimising the combined mean-squared error in log10-space against both the Churazov et al. (2021) X-ray profile and the Planck Collaboration et al. (2013) Compton-𝑦 profile. Left: Compton-𝑦 vs 𝑟/𝑅500𝑐, compared with Planck Collaboration et al. (2013) and Churazov et al. (2021). Right: X-ray surface brightness vs angular radius, compared with… view at source ↗
Figure 13
Figure 13. Figure 13: Azimuthally averaged entropy profiles 𝐾 (𝑟 ) = 𝑘𝑇/𝑛 2/3 𝑒 for all 50 realisations, plotted against 𝑟/𝑅500𝑐. Top: each profile coloured by the central Compton-𝑦 value inside 𝑟 < 0.05 𝑅500𝑐. Bottom: same but coloured by central X-ray surface brightness. Cool-core clusters (low central 𝐾) drive the high-brightness tail in both observables. as the redshift at which the main progenitor first reached 10% of its… view at source ↗
Figure 14
Figure 14. Figure 14: Correlation between the innermost-bin entropy 𝐾core (𝑟/𝑅200𝑐 ≈ 0.005, ∼10 kpc physical) and central brightness measured inside 𝑟 < 0.05 𝑅500𝑐. Left: 𝐾core vs central Compton-𝑦. Right: 𝐾core vs central X-ray surface brightness. Text annotations give the Pearson and Spearman correlation coefficients. The log 𝐾core–log SB𝑋 correlation is particularly strong (𝑟 = −0.87, 𝜌 = −0.80), confirming that central ent… view at source ↗
Figure 15
Figure 15. Figure 15: Entropy profiles for all 50 realisations, split two ways. Left: physical CC threshold — CC (blue, 𝑁 = 16) = 𝐾 < 200 keV cm2 at some 𝑟 < 0.1 𝑅200𝑐; non-CC (red, 𝑁 = 34) otherwise. Right: formation-time terciles by 𝑧 𝑓 (10%) (the redshift at which the main progenitor first reached 10% of its final 𝑀200𝑐) — early formers (blue), late formers (red), middle tercile (grey). Individual profiles thin; per-group m… view at source ↗
Figure 16
Figure 16. Figure 16: Mass accretion history for the host halo (left) and for the central BCG black hole (right), split by low-entropy (blue) and high-entropy (red). Top panels show the mass 𝑀(𝑧); bottom panels the accretion rate 𝑀¤ (𝑧). The thin lines represent individual clusters and the bold lines are the sample medians. Low-entropy progenitors reach 10% of 𝑀200𝑐 (𝑧 = 0) ∼1.3 Gyr earlier than high-entropy progenitors and ha… view at source ↗
Figure 17
Figure 17. Figure 17: Mean number of FoF mergers per cluster per redshift bin, split into four mass-ratio classes: major (𝑟 ≥ 1/3), minor (1/10 ≤ 𝑟 < 1/3), mini (1/100 ≤ 𝑟 < 1/10), and smooth (𝑟 < 1/100). Low-entropy clusters (blue) and high-entropy clusters (red) are shown with Poisson error bars. Redshift bins: [0, 0.5], [0.5, 1], [1, 2], [2, 4], [4, 8]; 𝑧 = 0 on the right. The mini-merger channel significantly distinguishes… view at source ↗
Figure 18
Figure 18. Figure 18: Entropy profiles split by mass-growth mode. Soft-grown clusters (blue, 𝑁 = 18) have accreted more than 60% of their 𝑀200𝑐 (𝑧 = 0) through mini mergers (1/100 ≤ 𝑟 < 1/10) plus smooth accretion (𝑟 < 1/100); merger-grown (red, 𝑁 = 32) are the rest. The soft-grown subset is 67% low￾entropy clusters (12/18) and covers 75% of all low-entropy clusters, making this the most effective low-entropy cluster predictor… view at source ↗
Figure 19
Figure 19. Figure 19: Example cluster that shows rapid change in the radial profiles in the last 500 Myrs through late mass assembly (Coma_042). Left: Compton-𝑦 profile vs 𝑟/𝑅500𝑐 with Planck Collaboration et al. (2013) data overlaid. Right: X-ray surface brightness vs arcmin with Churazov et al. (2021) data. The colour coded lines represent the time evolution of the cluster within the last 500 Myrs. For this particular cluste… view at source ↗
Figure 20
Figure 20. Figure 20: Projected maps of the 10 best-fitting realisations (same combined ranking as [PITH_FULL_IMAGE:figures/full_fig_p021_20.png] view at source ↗
Figure 21
Figure 21. Figure 21: Kernel density estimate of the 𝑀200𝑐 halo mass distribution across all 50 constrained Coma realisations. The light blue shaded curve shows the full distribution. Coloured dashed vertical lines mark the masses of the 10 best-fitting clusters (same combined ranking as in [PITH_FULL_IMAGE:figures/full_fig_p022_21.png] view at source ↗
read the original abstract

We present a suite of 50 high-fidelity simulations of Coma cluster analogues constructed from BORG/MANTICORE constrained initial conditions and evolved with the IllustrisTNG galaxy formation model. Regions predicted to form massive clusters comparable to Coma in mass and environment are selected and followed through cosmic time, producing realistic galaxy populations and intracluster medium properties. The ensemble captures both cosmic variance and uncertainties in the local initial conditions, providing a statistically robust framework for interpreting Coma in a cosmological context. We focus on direct comparisons with observed thermodynamical profiles of the intracluster medium. Specifically, we extract X-ray surface brightness profiles from the simulated clusters and confront them with measurements from eROSITA, as well as compute the thermal Sunyaev--Zel'dovich effect via integrated Compton-$y$ profiles for comparison with Planck satellite data. The simulations reproduce the broad shape and normalisation of both observables, while also highlighting the range of scatter expected from environmental and assembly history differences. This enables us to assess how feedback processes, merger activity, and large-scale environment shape observable cluster properties. Our results demonstrate that combining constrained cosmological initial conditions with state-of-the-art galaxy formation physics provides an effective strategy for generating targeted, observation-driven analogues of specific clusters. The resulting dataset offers a valuable resource for testing models of intracluster medium physics, calibrating scaling relations, and interpreting upcoming joint X-ray and Sunyaev--Zel'dovich observations of nearby massive clusters.

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

1 major / 2 minor

Summary. The paper presents a suite of 50 high-fidelity simulations of Coma cluster analogues constructed from BORG/MANTICORE constrained initial conditions and evolved with the IllustrisTNG galaxy formation model. Regions predicted to form massive clusters comparable to Coma are selected and followed, with direct comparisons of extracted X-ray surface brightness profiles to eROSITA measurements and integrated Compton-y profiles to Planck data. The central claim is that the simulations reproduce the broad shape and normalisation of both observables while capturing the range of scatter expected from environmental and assembly history differences, demonstrating the utility of constrained ICs plus state-of-the-art galaxy formation physics for generating targeted cluster analogues.

Significance. If the result holds, the work provides a statistically robust ensemble framework for interpreting a specific observed cluster (Coma) in a cosmological context, accounting for cosmic variance and initial-condition uncertainties. This is valuable for testing ICM physics models, calibrating scaling relations, and preparing for joint X-ray/SZ observations, as the constrained approach directly ties simulations to observed large-scale structure.

major comments (1)
  1. [Abstract] The abstract states that the simulations 'reproduce the broad shape and normalisation' of the X-ray and Compton-y profiles but supplies no quantitative metrics (e.g., reduced chi-squared, fractional residuals, or profile-by-profile comparisons with error bars), making it impossible to evaluate how well the claim is supported or how the scatter is quantified relative to the data.
minor comments (2)
  1. Clarify the precise selection criteria used to identify the 50 Coma analogues from the BORG/MANTICORE volume (e.g., mass range, environmental metrics, or matching tolerances).
  2. Specify the radial range, binning, and projection method employed when extracting the simulated X-ray surface brightness and Compton-y profiles for direct comparison to the observational datasets.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive review and recommendation for minor revision. We address the single major comment below.

read point-by-point responses

  1. Referee: [Abstract] The abstract states that the simulations 'reproduce the broad shape and normalisation' of the X-ray and Compton-y profiles but supplies no quantitative metrics (e.g., reduced chi-squared, fractional residuals, or profile-by-profile comparisons with error bars), making it impossible to evaluate how well the claim is supported or how the scatter is quantified relative to the data.

    Authors: We agree that the abstract, in its current form, lacks quantitative metrics to support the reproduction claim. The main text provides detailed comparisons, including profile-by-profile assessments against eROSITA and Planck data along with explicit quantification of scatter due to environment and assembly history (see Figures 3–5 and Sections 3–4). To address the referee’s point, we will revise the abstract to include a concise quantitative statement referencing these results, such as the typical fractional residuals or consistency within the expected scatter. This is a straightforward minor change. revision: yes

Circularity Check

0 steps flagged

No significant circularity identified

full rationale

The paper constructs an ensemble of constrained simulations from BORG/MANTICORE initial conditions evolved under the IllustrisTNG model, then extracts X-ray surface brightness and integrated Compton-y profiles for direct comparison against independent external datasets from eROSITA and Planck. No load-bearing equations, fitted parameters renamed as predictions, self-definitional relations, or self-citation chains appear in the provided text that would reduce the reported reproduction of broad shapes and scatter to the simulation inputs by construction. The central claim remains an external validation exercise against separate observational measurements, rendering the derivation self-contained.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on two domain assumptions whose validity is not demonstrated within the abstract: the accuracy of the constrained initial conditions for reproducing Coma and the suitability of IllustrisTNG for the intracluster medium.

axioms (2)
  • domain assumption BORG/MANTICORE constrained initial conditions accurately select regions that form Coma-like clusters in mass and environment.
    Used to construct the 50 simulation initial conditions from which the cluster analogues are drawn.
  • domain assumption The IllustrisTNG galaxy formation model produces realistic intracluster medium properties for the X-ray and Compton-y comparisons.
    The simulations are evolved with this model to generate the galaxy populations and ICM used for the profile extractions.

pith-pipeline@v0.9.1-grok · 5855 in / 1395 out tokens · 26872 ms · 2026-06-27T15:14:45.664803+00:00 · methodology

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