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arxiv: 2606.19443 · v1 · pith:YDOAM4Y5new · submitted 2026-06-17 · 🌌 astro-ph.CO · astro-ph.GA

The impact of evolving cosmic filaments on mass and spin evolution of dark matter halos

Hannah Jhee , Hyunmi Song , Clotilde Laigle , Christophe Pichon , Corentin Cadiou , Ena Choi This is my paper

Pith reviewed 2026-06-26 19:42 UTC · model grok-4.3

classification 🌌 astro-ph.CO astro-ph.GA
keywords cosmic filamentsdark matter halosmass accretion ratespin alignmentlarge-scale structureN-body simulationsfilament evolutionenvironmental effects
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The pith

Halos approaching dense filaments see suppressed mass accretion from the outskirts and non-random spin alignments.

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

This paper develops an algorithm to trace the progenitors of cosmic filaments identified at the present day by measuring spatial similarity to candidates at earlier times. Using this, it reconstructs how filaments drift and change density, then examines halos in a reference frame that moves with each filament. The analysis reveals that halos experience reduced mass growth when nearing high-density filaments, with the effect starting at the outer regions. Spin alignments of halos also evolve differently than expected from random processes alone. By excluding major mergers, the study isolates the dynamical influence of the filament environment on halo properties.

Core claim

Reconstructing the evolutionary histories of individual filaments through spatial similarity matching allows halo phase-space trajectories to be analyzed in a time-evolving filament-centric frame. This shows that mass accretion rates onto halos are systematically suppressed as they approach high-density filaments, beginning at the filament outskirts. The evolution of halo spin alignments departs from stochastic random-walk expectations, suggesting that distinct mass flow regimes around filaments apply different torques to infalling halos.

What carries the argument

An algorithm tracing filament progenitors via spatial similarity quantification, which reconstructs bulk drift and density evolution to create a dynamic filament-centric frame separating halo motions from filament motions.

If this is right

  • Mass accretion rates are suppressed beginning at filament outskirts, suggesting tidal stripping or reduced net accretion.
  • Halo spin alignments depart from random-walk expectations due to torques from anisotropic flows.
  • Filament properties like splashback radii and core overdensities can be tracked over time.
  • Environmental effects are characterized without contamination from major mergers.
  • Simultaneous tracking of filaments and halos is required for accurate description of large-scale influences.

Where Pith is reading between the lines

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

  • Galaxy formation simulations may need to incorporate time-dependent filament environments to predict accurate mass assembly histories.
  • The observed spin changes could be tested using weak lensing or galaxy shape measurements around filaments.
  • Applying the tracing method to other cosmic web elements could reveal similar environmental impacts.
  • This approach might help reconcile discrepancies between observed and simulated halo properties in dense regions.

Load-bearing premise

The spatial similarity algorithm correctly identifies filament progenitors and reconstructs their histories including drift and density changes without major biases.

What would settle it

If mass accretion rates measured in an evolving filament frame do not show suppression starting at the outskirts of high-density filaments, or if spin alignments follow random walks, the central findings would be falsified.

Figures

Figures reproduced from arXiv: 2606.19443 by Christophe Pichon, Clotilde Laigle, Corentin Cadiou, Ena Choi, Hannah Jhee, Hyunmi Song.

Figure 1
Figure 1. Figure 1: The smoothed density significance map of a slab of Δ𝑦 ∼ 4.2 ℎ −1 Mpc at 𝑧 = 0, 1, 2 and 3, around the most massive cluster. Peaks and saddle critical points within the slab are shown as red triangles and green crosses respectively, and filament segments also within the slab are shown as red lines. Here, the -cut parameter to filter low-contrast filaments was set to 1. The black crosses and black dashed lin… view at source ↗
Figure 2
Figure 2. Figure 2: Spatial distribution of the 72 filaments at 𝑧 = 0 whose progenitors have been traced back to 𝑧 > 1. The red sphere at the center denotes a radius of 2𝑅vir from each cluster center at 𝑧 = 0; the three clusters have virial radii of 1.58, 1.57, and 1.56 cMpc/ℎ, respectively. Filaments at 𝑧 = 0 are shown in blue, while filaments at higher redshift are shown as progressively red. MNRAS 000, 1–14 (2025) [PITH_F… view at source ↗
Figure 3
Figure 3. Figure 3: The peculiar drift velocities of the three filaments around the third most massive cluster, shown as a function of cosmic time. The velocities are measured at three critical points: two nodes (shaded regions) and one saddle point (dashed lines). The shaded regions between the two curves illustrate the ranges of velocity variation between the two nodes, while the dotted lines denote the velocities measured … view at source ↗
Figure 4
Figure 4. Figure 4: Left: The overdensity profiles at all redshifts of one filament are shown in the top panel, and the slope 𝛾 = 𝑑 log 𝜌/𝑑 log 𝑑fil in the bottom panel. In each panel, the red curve corresponds to 𝑧 = 3 and the blue one to 𝑧 = 0. The splashback radius is defined as the radius minimizing 𝛾. Middle: The evolution of the splashback radii of 72 filaments are shown as thin gray lines. The average is shown as black… view at source ↗
Figure 5
Figure 5. Figure 5: For six halos around one of the 72 filaments, the distance from halos to filaments is shown as a function of cosmic time (bottom label) or redshift (top label). The faint solid lines indicate the distances assuming the filament positions are fixed at 𝑧 = 0, while opaque dashed curves are measured using the positions of the filament progenitors. Because the curves are noisy, we also smoothed the trajectorie… view at source ↗
Figure 6
Figure 6. Figure 6: The comparison between the absolute velocity components along the filaments, 𝑣 abs fh = v3D · 𝑢ˆfh (𝑧), and the relative velocity, 𝑣 rel fh = 𝑎 · 𝑑(𝑑fh )/𝑑𝑡. The black diagonal line marks the one-to-one relation. The un￾derlying distribution is shown as black contours, with five levels equally spaced in logarithmic scale between 10 and 220. The colors of hexagonal bins show the median normalized distances.… view at source ↗
Figure 9
Figure 9. Figure 9: Halo spin–filament alignment as a function of the normalized halo–filament separation, 𝑑fh/𝑅spb. Halos are subdivided at 𝑧 = 0 into a “parallel” sample (red) with | ˆ𝑗 · 𝑢ˆfil | > 0.5 and a “perpendicular” sample (blue) with | ˆ𝑗 · 𝑢ˆfil | < 0.5. The observed tuning-fork–like separation is compared to a null model in which halo spins evolve stochastically as an isotropic random walk on the sphere (gray reg… view at source ↗
read the original abstract

The evolution of galaxies is closely tied to that of their host dark matter halos, which is in turn strongly modulated by the surrounding large-scale environment. Cosmic filaments are expected to influence the peculiar motions, mass assembly and angular momentum of nearby halos through highly anisotropic matter flows. In order to fully capture the dynamic interplay between the filaments and halos, we develop an algorithm to trace the progenitors of individual filaments identified at z=0 with DisPerSE in a cosmological N-body simulation, by quantifying the spatial similarity between a descendant filament and progenitor candidates. This enables us to reconstruct filament-by-filament evolutionary histories, including their bulk drift and the evolution of density profiles, from which splashback radii and core overdensities are derived. Using these time-dependent properties, we re-examine halo phase-space trajectories in a filament-centric frame that evolves with time. This eliminates biases inherent to static models by separating halo motions from the motion of the filaments, allowing trajectories to be identified more reliably. We find that as halos approach high-density filaments, their mass accretion rates are systematically suppressed beginning at the filament outskirts, suggestive of tidal stripping or suppressed net accretion. Furthermore, the evolution of halo spin alignments exhibits a clear departure from stochastic random-walk expectations. This suggests that distinct mass flow regimes in and around filaments exert different torques on infalling halos, thereby changing their angular momentum. Our findings, derived from a sample screened for major mergers, highlight the pure dynamical impact of the filamentary environment. Ultimately, we demonstrate that tracking the simultaneous co-evolution of filaments and halos is essential for accurately characterizing environmental effects.

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

3 major / 1 minor

Summary. The paper develops an algorithm to trace progenitors of z=0 filaments identified with DisPerSE in cosmological N-body simulations by quantifying spatial similarity between descendant and candidate filaments. This reconstructs filament evolutionary histories including bulk drift and density profile evolution, from which splashback radii and core overdensities are derived. Halos are then analyzed in a time-evolving filament-centric frame to separate their motions from filament motion. The central findings are that mass accretion rates are systematically suppressed as halos approach high-density filaments, beginning at the outskirts (suggestive of tidal stripping or suppressed accretion), and that halo spin alignments depart from stochastic random-walk expectations, indicating distinct torques from filamentary mass flows. The sample is screened for major mergers to isolate pure dynamical effects.

Significance. If the filament-tracing procedure is shown to be unbiased, the work demonstrates the necessity of co-evolving filaments and halos to avoid biases from static environmental models, providing direct evidence for environmental modulation of halo mass assembly and angular momentum via anisotropic flows. The approach uses raw simulation outputs without fitted parameters and yields falsifiable predictions about accretion suppression and spin evolution that can be tested in other simulations or observations. This has implications for galaxy formation models that incorporate filamentary environments.

major comments (3)
  1. [Methods] Methods (filament progenitor tracing): The spatial similarity algorithm for matching descendant filaments to progenitors is described but supplies no quantitative validation, such as recovery fractions on controlled test cases, sensitivity analysis to the similarity threshold, or cross-checks against alternative tracers (e.g., density peak tracking). This is load-bearing for the central claims because systematic mismatches in bulk drift or density gradients would shift the inferred filament outskirts and splashback radii, directly altering the reported accretion-rate suppression and spin-alignment results.
  2. [Results] Results (mass accretion rates): The claim of systematic suppression beginning at filament outskirts lacks reported error bars, sample statistics (number of halos per filament density bin), and explicit controls confirming that the screening for major mergers fully removes merger-driven accretion signals. Without these, it is unclear whether the suppression is statistically robust or could be influenced by residual selection effects.
  3. [Results] Results (spin alignments): The departure from stochastic random-walk expectations is stated but the quantitative measure (e.g., the specific statistic or model for the random-walk null hypothesis) and its significance level are not detailed in the provided description, making it difficult to assess whether the departure is load-bearing or could arise from the evolving frame definition itself.
minor comments (1)
  1. [Abstract/Methods] The abstract and methods would benefit from a brief statement of the similarity metric's functional form (e.g., whether it is a simple overlap integral or includes density weighting) to aid reproducibility.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the constructive and detailed report. We address each major comment below and will revise the manuscript to incorporate the suggested improvements.

read point-by-point responses

  1. Referee: [Methods] Methods (filament progenitor tracing): The spatial similarity algorithm for matching descendant filaments to progenitors is described but supplies no quantitative validation, such as recovery fractions on controlled test cases, sensitivity analysis to the similarity threshold, or cross-checks against alternative tracers (e.g., density peak tracking). This is load-bearing for the central claims because systematic mismatches in bulk drift or density gradients would shift the inferred filament outskirts and splashback radii, directly altering the reported accretion-rate suppression and spin-alignment results.

    Authors: We agree that the current manuscript lacks explicit quantitative validation of the progenitor-tracing algorithm. In the revised version we will add a dedicated subsection (or appendix) presenting recovery fractions from controlled test cases with injected filament evolutions, a sensitivity analysis on the similarity threshold, and direct comparisons against density-peak tracking. These additions will demonstrate that the algorithm does not introduce systematic biases capable of altering the reported accretion and spin results. revision: yes

  2. Referee: [Results] Results (mass accretion rates): The claim of systematic suppression beginning at filament outskirts lacks reported error bars, sample statistics (number of halos per filament density bin), and explicit controls confirming that the screening for major mergers fully removes merger-driven accretion signals. Without these, it is unclear whether the suppression is statistically robust or could be influenced by residual selection effects.

    Authors: The manuscript already applies a major-merger screen to isolate dynamical effects, but we acknowledge that error bars, per-bin halo counts, and explicit validation of the screen are not presented with sufficient detail. The revision will include error bars on all accretion-rate measurements, tabulate the number of halos per filament-density bin, and add a supplementary test (e.g., comparison of screened versus unscreened samples) confirming that residual merger-driven accretion is negligible. revision: yes

  3. Referee: [Results] Results (spin alignments): The departure from stochastic random-walk expectations is stated but the quantitative measure (e.g., the specific statistic or model for the random-walk null hypothesis) and its significance level are not detailed in the provided description, making it difficult to assess whether the departure is load-bearing or could arise from the evolving frame definition itself.

    Authors: We will expand the spin-alignment section to specify the exact statistic employed, the precise random-walk null model (including how the evolving filament-centric frame is accounted for), and the numerical significance level of the observed departure. This clarification will allow readers to evaluate whether the result is robust against frame-definition artifacts. revision: yes

Circularity Check

0 steps flagged

No circularity: results from direct simulation analysis with novel algorithm

full rationale

The paper develops a new spatial-similarity algorithm to trace filament progenitors in N-body simulation data, then applies it to re-express halo trajectories in an evolving filament-centric frame. No quoted step reduces a claimed result to a fitted parameter renamed as prediction, a self-citation chain, or a self-definitional equivalence. The central findings (suppressed accretion rates and non-random spin evolution) are presented as empirical outputs from the screened simulation sample, with the algorithm described as an original contribution rather than imported via prior self-citation. The derivation chain therefore remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The work rests on the reliability of the spatial similarity matching for filament tracing and standard assumptions of N-body simulations; no free parameters or invented entities are described in the abstract.

axioms (1)
  • domain assumption The spatial similarity metric accurately identifies true filament progenitors across simulation snapshots.
    This underpins the entire reconstruction of filament evolutionary histories described in the abstract.

pith-pipeline@v0.9.1-grok · 5846 in / 1140 out tokens · 31602 ms · 2026-06-26T19:42:39.754909+00:00 · methodology

discussion (0)

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Reference graph

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