arxiv: 2604.26022 · v2 · submitted 2026-04-28 · 🌌 astro-ph.CO

Recognition: unknown

Secondary Dependence of Baryonic Effects on the Density Profile of Dark Matter Halos

Yikun Wang , Idit Zehavi , Sergio Contreras , Giovanni Aric\`o , Sownak Bose , Lars Hernquist

Authors on Pith no claims yet

Pith reviewed 2026-05-07 14:43 UTC · model grok-4.3

classification 🌌 astro-ph.CO

keywords baryonic effectsdark matter halosdensity profileshalo concentrationsecondary halo propertiescosmological simulationslarge scale structurefeedback effects

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The pith

Baryonic effects on dark matter halo density profiles show strong secondary dependence on concentration at fixed mass.

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

The paper investigates variations in how baryons alter the density profiles of dark matter halos depending on secondary properties such as concentration and environment, while keeping halo mass fixed. It finds that at the current epoch, concentration has a notable effect particularly for lower mass halos, where higher concentration leads to less pronounced increases in central density and more suppression at intermediate radii, with changes up to about 15 percent. This dependence is weaker for the large-scale environment around the halo. The effects continue at earlier times and relate to differences in the baryonic content within the halos. Understanding these variations matters because baryonic physics introduces uncertainties in cosmological surveys that use halo profiles to infer structure growth.

Core claim

At redshift zero, the ratio of density profiles from hydrodynamical and dark-matter-only simulations depends on halo concentration at fixed mass, with more concentrated low-mass halos showing weaker inner enhancement and stronger suppression at intermediate radii. Variations reach approximately 15 percent on small scales and lessen at larger radii. The trend reverses at higher masses. Large-scale environment shows only about 2 percent dependence that is mostly scale-independent. Concentration affects both internal redistribution and total mass suppression, while environment primarily shifts the overall mass. These secondary dependencies persist to redshift 0.5 and connect to variations in内部b

What carries the argument

The ratio of hydro to dark-matter-only density profiles for mass-matched halos, analyzed as a function of secondary halo properties.

Load-bearing premise

Halos can be accurately paired between the hydrodynamical and dark-matter-only versions and that the simulation's treatment of baryonic processes correctly represents their effect on dark matter distribution in nature.

What would settle it

Measuring the inner and intermediate density profiles of low-mass galaxy groups split by concentration and comparing the ratio to dark-matter-only expectations from observations.

read the original abstract

Baryonic physics is anticipated to be a major source of systematic uncertainty in current and future large-scale cosmological surveys. We investigate how baryonic effects on halo density profiles vary with secondary halo properties at fixed halo mass, using the large-volume MillenniumTNG hydrodynamical simulation and its dark matter-only counterpart. We focus on the impact of halo concentration and large-scale environment on the ratio of density profiles of matched halos in the hydrodynamical and dark matter-only simulations. At redshift $z = 0.0$, we find a strong dependence on halo concentration, especially at lower halo mass ($12.5 < \log(M_h/h^{-1}M_{\odot}) < 13.0$), where more concentrated halos exhibit weaker inner enhancement and stronger intermediate-radius suppression at fixed halo mass, with variations reaching $\sim 15\%$ at small scales and decreasing toward larger scales. This trend weakens and reverses at higher halo mass. In contrast, the secondary dependence on large-scale environment is weaker ($\sim 2\%$) and largely scale-independent, with halos in denser regions exhibiting slightly weaker intermediate suppression. By separating internal profile redistribution from total mass suppression, we show that concentration impacts both components, whereas the environmental dependence is primarily associated with an overall mass shift. These secondary dependencies persist at $ z = 0.5$ and correlate with variations in internal baryonic properties. We examine additional halo properties, including halo spin and velocity dispersion, and find significant secondary dependence. Overall, our results highlight the important role of secondary halo properties in modulating baryonic effects on halo density profiles, with potential implications for future modeling efforts.

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.

Desk Editor's Note private letter to a colleague

The paper gives concrete numbers on how concentration drives ~15% secondary variation in baryonic profile changes at low halo mass, with environment at ~2%, plus a clean split between internal redistribution and mass loss.

read the letter

The main thing to know is that baryonic effects on dark matter density profiles are not uniform at fixed mass. At z=0, more concentrated halos show weaker inner boosts and stronger suppression around intermediate radii, with the difference hitting 15% at small scales for halos around 10^12.5-13 solar masses. The environmental signal is smaller and flatter. They also separate the profile shape change from the overall mass suppression, which is a useful split. These trends hold at z=0.5 and tie to baryonic properties inside the halos. Spin and velocity dispersion show secondary dependence too. The large MillenniumTNG volume and matched-halo approach make the statistics reliable enough to report specific percentages rather than just qualitative trends. That decomposition and the mass-dependent reversal at higher masses are the clearest additions over earlier work on baryonic back-reaction. The results are directly usable for updating halo models in survey analyses. The matching between hydro and dark-matter-only runs is the part that needs the most attention. Any concentration-dependent bias in how SUBFIND pairs objects could mimic or exaggerate the 15% signal, and the abstract does not spell out the matching tolerances or success rates broken down by secondary properties. If the full methods section shows that matching quality is uniform, the claim strengthens; otherwise the concentration trend is harder to interpret cleanly. This is the kind of paper that belongs in a reading group focused on baryonic systematics or halo modeling. People building emulators or fitting functions for large-scale structure will find the numbers worth pulling out. It is solid enough to send to referees, though they will likely ask for more diagnostics on the matching and error bars on the secondary trends.

Referee Report

2 major / 3 minor

Summary. The manuscript uses the MillenniumTNG hydrodynamical simulation and its dark-matter-only counterpart to quantify secondary dependencies of baryonic effects on dark matter halo density profiles at fixed halo mass. By matching halos between the two runs, the authors report a strong dependence on halo concentration (especially for 12.5 < log(M_h/h^{-1}M_⊙) < 13.0), with more concentrated halos showing weaker inner enhancement and stronger intermediate-radius suppression (variations ~15% at small scales). Environmental dependence is weaker (~2%) and largely scale-independent. The study separates internal profile redistribution from total mass suppression, demonstrates persistence of trends at z=0.5, and examines correlations with internal baryonic properties as well as additional halo properties such as spin and velocity dispersion.

Significance. If the secondary dependencies hold after detailed validation, the work shows that baryonic modifications to halo density profiles are modulated by concentration and other properties rather than being universal at fixed mass. This has direct relevance for reducing systematic uncertainties in weak-lensing and galaxy-clustering analyses. The large-volume matched-halo comparison is a standard and appropriate method that provides good statistical power; the decomposition into internal redistribution versus overall mass loss is a useful distinction, and the correlation with internal baryonic properties adds physical insight.

major comments (2)

[§4.1] §4.1 (Halo matching procedure): The reported concentration dependence at low mass is load-bearing on the fidelity of halo matching between hydro and DMO runs. The manuscript describes the matching algorithm and reports overall success rates, but does not test whether success rates, center offsets, or mass-loss distributions vary systematically with concentration or environment. If baryonic contraction shifts centers more for concentrated halos, SUBFIND pairing could imprint an artificial trend on the hydro/DMO density ratio; a supplementary figure showing matching quality binned by concentration bin is needed to confirm the trend is physical.
[§5.2] §5.2 and Figure 5 (Error estimation and sample sizes): The ~15% variations are presented with error bars whose construction is not fully detailed. It is unclear whether the uncertainties incorporate the paired nature of the data, covariance across radial bins, or the finite number of matched pairs per concentration bin. Without this, the statistical significance of the concentration-driven differences (and their reversal at higher mass) cannot be fully assessed.

minor comments (3)

[Abstract] Abstract: The mass bin 12.5 < log(M_h/h^{-1}M_⊙) < 13.0 is stated without specifying the exact bin width or number of halos per bin; adding this would improve reproducibility.
[Figure captions] Figure captions (e.g., Figure 3): The radial range over which the ~15% variation is measured should be stated explicitly (e.g., r < 0.1 R_200) rather than only 'small scales'.
[§6] §6 (Discussion): A brief comparison to earlier works on baryonic effects on the mass-concentration relation would better highlight the novelty of the secondary-dependence results.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for the constructive comments. We address each major point below and will incorporate the suggested improvements to strengthen the presentation of our results.

read point-by-point responses

Referee: [§4.1] §4.1 (Halo matching procedure): The reported concentration dependence at low mass is load-bearing on the fidelity of halo matching between hydro and DMO runs. The manuscript describes the matching algorithm and reports overall success rates, but does not test whether success rates, center offsets, or mass-loss distributions vary systematically with concentration or environment. If baryonic contraction shifts centers more for concentrated halos, SUBFIND pairing could imprint an artificial trend on the hydro/DMO density ratio; a supplementary figure showing matching quality binned by concentration bin is needed to confirm the trend is physical.

Authors: We agree that demonstrating the robustness of the halo-matching procedure with respect to concentration is essential, particularly for the low-mass bin where the secondary dependence is strongest. In the revised manuscript we will add a supplementary figure showing matching success rates, center offsets, and mass-loss distributions binned by concentration (and, for completeness, by environment). This will confirm that the reported trends are not driven by systematic differences in matching quality. revision: yes
Referee: [§5.2] §5.2 and Figure 5 (Error estimation and sample sizes): The ~15% variations are presented with error bars whose construction is not fully detailed. It is unclear whether the uncertainties incorporate the paired nature of the data, covariance across radial bins, or the finite number of matched pairs per concentration bin. Without this, the statistical significance of the concentration-driven differences (and their reversal at higher mass) cannot be fully assessed.

Authors: We acknowledge that the current description of the error estimation is insufficiently detailed. The error bars are obtained via bootstrap resampling of the matched halo pairs within each concentration bin, which accounts for the paired nature of the hydro-DMO comparison. In the revised manuscript we will expand §5.2 to describe the bootstrap procedure explicitly, state the number of matched pairs per bin, and clarify how any radial-bin covariance is (or is not) incorporated. We will also report the sample sizes in the figure caption to allow readers to assess statistical significance directly. revision: yes

Circularity Check

0 steps flagged

No significant circularity in empirical simulation analysis

full rationale

The paper performs a direct empirical comparison of halo density profiles between the MillenniumTNG hydrodynamical simulation and its dark-matter-only counterpart, quantifying ratios and secondary dependencies on concentration and environment for matched halos. No derivations, model equations, fitted parameters repurposed as predictions, or self-referential definitions appear in the presented results. The measurements of ~15% variations and mass redistribution are computed from simulation outputs without any load-bearing self-citation chains, ansatzes, or uniqueness theorems that reduce the central claims to inputs by construction. The study is self-contained as a data-driven analysis.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the fidelity of the hydrodynamical simulation and the validity of the halo-matching procedure; these are standard domain assumptions rather than new postulates.

axioms (1)

domain assumption The MillenniumTNG hydrodynamical model accurately captures the net effect of baryonic processes on dark matter halo profiles.
Invoked when interpreting differences between hydro and DMO runs as physical baryonic effects.

pith-pipeline@v0.9.0 · 5619 in / 1247 out tokens · 58902 ms · 2026-05-07T14:43:50.677199+00:00 · methodology

discussion (0)

Reference graph

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