Pith. sign in

REVIEW 3 major objections 4 minor 72 references

A circumsphere filter on tiled Delaunay tessellations lets DisPerSE scale to gigaparsec simulations.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · deepseek-v4-flash

2026-08-02 01:02 UTC pith:RCAWZ2UU

load-bearing objection A genuinely useful tiling method for DisPerSE with solid validation, but the abstract oversells the connectivity result and the validation reference is not the true global tessellation. the 3 major comments →

arxiv 2607.14785 v2 pith:RCAWZ2UU submitted 2026-07-16 astro-ph.GA astro-ph.CO

Enabling Cosmic Web Analysis at Gigaparsec Scales: A Multi Block Approach for DisPerSE

Ankit Singh , Frazer Pearce , Meghan Gray , Gustavo Yepes This is my paper
classification astro-ph.GA astro-ph.CO
keywords cosmic webfilament detectionDisPerSEDelaunay tessellationlarge-scale structureN-body simulationconnectivitypersistence
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper claims that the memory bottleneck preventing DisPerSE from processing gigaparsec simulations can be broken by tiling the volume into overlapping blocks and keeping only tetrahedra whose circumspheres lie entirely within each padded tile. Because a tetrahedron with its circumsphere fully inside the padded region is guaranteed to belong to the global Delaunay tessellation, the filtered tiled tessellation matches the monolithic one almost exactly. Validation on a 300 Mpc/h subvolume shows 99.6% recovery of total filament length, 100% of density maxima and minima, and 94.7% of individual filaments. The method is then applied to the full 1 Gpc MDPL2 box with 92 million haloes, producing the first gigaparsec-scale filament catalogue from a topologically rigorous N-body analysis, and a measurement of the halo mass-connectivity relation with slope A≈0.27–0.315.

Core claim

The central discovery is that a tetrahedron whose circumsphere fits entirely within a padded tile is provably part of the global Delaunay tessellation, so overlapping tiles can be filtered by this circumsphere criterion and merged to reproduce the monolithic result almost exactly. On a 300 Mpc/h subvolume of MDPL2, the tiled pipeline recovers 99.6% of the total filament length, 100% of density maxima and minima, 99.7% of 2-saddles, and 94.7% of individual filaments, with zero spurious critical points. The approximately 5% unmatched filaments are predominantly short, low-significance structures. The method is applied to the full 1 Gpc MDPL2 box, and as a first science application the authors

What carries the argument

The central object is the circumsphere of a Delaunay tetrahedron. The empty-circumsphere property defines global validity: a tetrahedron belongs to the global Delaunay tessellation if no other input point lies inside its circumsphere. By padding each tile with a layer whose width is set from the circumradius distribution (60 Mpc/h for MDPL2, capturing 99.33% of tetrahedra) and discarding tetrahedra whose circumspheres cross the padded boundary, the surviving 'frozen core' tetrahedra are guaranteed identical to the monolithic tessellation. A post-processing pipeline with a single tolerance parameter δ=0.5 Mpc/h then deduplicates and stitches filaments across tile boundaries.

Load-bearing premise

The monolithic reference run with 60 Mpc/h padding is treated as the true global cosmic-web topology, even though rare void tetrahedra have circumspheres extending to 273 Mpc/h or more, so points outside that padding could alter the reference tessellation itself.

What would settle it

Run the frozen-core tiled pipeline on a larger reference volume (e.g., a 500 Mpc/h core with 200 Mpc/h padding, or a fully periodic 1 Gpc box) and compare the tiled output against that monolithic result; if the 99.6% length recovery and 94.7% filament matching degrade when the reference padding is increased, the original reference was not the true global tessellation.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • DisPerSE can now be applied to next-generation simulations with 10^8–10^9 tracer objects, such as Euclid Flagship and FLAMINGO volumes, using bounded memory per compute node.
  • Density maxima and minima are recovered at 100%, so node-based studies (cluster identification, void centres) can rely on the tiled catalogue as faithfully as on a monolithic run.
  • The mass-connectivity power law is confirmed in a pure dark-matter halo catalogue across three decades in halo mass, matching gas-based and persistent-homology slopes.
  • Filament catalogues at multiple persistence thresholds provide a quantitative reference for the length distribution and number density of the cosmic web in the largest volume analysed to date.
  • The method is embarrassingly parallel and scales to arbitrarily large volumes by increasing the number of tiles while keeping per-node memory constant.

Where Pith is reading between the lines

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

  • The circumsphere-filtering principle is not tied to DisPerSE; it could generalize to other Delaunay-based estimators, such as DTFE density fields or topological analyses of other point processes, wherever a global tessellation is assumed.
  • The padding width is set by the tracer's circumradius distribution and may become impractically large for sparse tracers with heavy tails, suggesting that for such data a probabilistic (rather than absolute) guarantee of global validity would need to be accepted.
  • The 5% unmatched short filaments, distributed throughout the volume rather than only at boundaries, indicate that the method is conservative by design; studies requiring exact per-filament fidelity around individual objects should still use monolithic runs on smaller regions.
  • The stability of the connectivity slope across persistence thresholds suggests that the mass-connectivity relation is a robust feature of the cosmic web topology, not an artifact of threshold choice, which could simplify comparisons between future surveys and simulations.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. The paper presents a frozen-core, multi-block method for running DisPerSE on gigaparsec-scale halo catalogues. The volume is split into overlapping tiles; each tile is padded and tessellated independently; a circumsphere filter retains only tetrahedra whose circumspheres lie entirely inside the padded tile, which are guaranteed to belong to the global Delaunay tessellation; a post-processing pipeline merges the tiled outputs via core filtering, KDTree-based deduplication, and boundary stitching. Validation against a monolithic reference run on a 300 Mpc/h MDPL2 subvolume reports 99.6% total filament-length recovery, 94.7% individual filament matching, and 100% recovery of density maxima and minima. The method is applied to the full (1 Gpc/h)^3 MDPL2 box with 92 million haloes, producing a Gpc-scale filament catalogue at three persistence thresholds. As an application, the paper measures the mass–connectivity relation for ~22,900 haloes from 10^12 to 10^15.5 M_sun/h, reporting a power-law slope A ≈ 0.27–0.315 at 1.5R200 and claiming agreement with gas-based and theoretical results.

Significance. If the claims are accurate, this is a practically important contribution: it removes the dominant memory bottleneck of DisPerSE and enables topologically rigorous filament extraction in volumes inaccessible to monolithic runs. The validation design is a genuine strength: a direct comparison against a monolithic reference, a systematic ablation of pipeline stages, and a public simulation/data set. The connectivity analysis is a useful first Gpc-scale halo-based measurement and the reported slope is consistent with independent gas-based and persistent-homology analyses. However, several headline claims — 'preserving global topology', 'across three decades', and 'first confirmation in an N-body halo catalogue' — overstate what is actually demonstrated and need to be corrected or qualified.

major comments (3)
  1. [§2.4.1, Table 1, §2.5.4, §4.2] The validation reference is itself a finite-padded approximation, not the true global Delaunay/Morse-Smale complex. The circumsphere criterion is one-directional: a tetrahedron whose circumsphere lies wholly inside the padded tile is globally valid, but the converse is not established. With P=60 Mpc/h capturing only 99.33% of tetrahedra and a 99.9th-percentile circumradius of 273 Mpc/h, a tail of tetrahedra has circumspheres extending beyond the padding; points in the rest of the 1 Gpc/h box could invalidate such tetrahedra. The monolithic reference uses the same P=60 Mpc/h and is therefore itself an approximation. The quoted 99.6% length and 94.7% filament recovery rates measure agreement with this P=60-specific reference, not with the global topology that the abstract claims to preserve. The paper partially concedes this in §4.2 ('to within the 0.37 per cent of tetrahedra whose circums
  2. [Abstract; §3.3.4; Fig. 13] The abstract claims the mass–connectivity relation 'extends ... across three decades in halo mass', but the paper itself states in §3.3.4 that 'The power-law relation holds over nearly two decades in halo mass above the κ > 2 threshold'. The fit uses only bins with mean κ > 2, so the range 10^12–10^15.5 M_sun/h is not fully covered by the fitted power law. This is a direct inconsistency between the abstract/conclusions and the actual fitted range. Revise the abstract and conclusions to 'nearly two decades' (or fit the full range and report the resulting slope).
  3. [Abstract; §3.3.5] The abstract's claim of 'the first confirmation in an N-body halo catalogue that the theoretically predicted scaling holds across three decades in halo mass' appears contradicted by the paper's own literature review. Section 3.3.5 states that Galárraga-Espinosa et al. (2024) 'measured connectivity from DisPerSE applied to the MillenniumTNG halo catalogue in a (500 h−1 Mpc)^3 box ... Their slopes are consistent with our values', and earlier work such as Colberg et al. (2005) also used N-body simulations. Unless 'first' is narrowly meant as 'first at Gpc scale' or 'first across a specific mass range', the novelty claim is inaccurate. Please specify precisely what is new and avoid a blanket 'first confirmation' statement.
minor comments (4)
  1. [Table 1 caption; §2.4.1] The text says the 60 Mpc/h padding captures 99.33% of tetrahedra, but the Table 1 caption says 'captures 99.3 per cent'. Unify the precision.
  2. [§2.4.2] The statement that 'the 60 Mpc/h padding used in our pipeline therefore provides ample margin' is too strong given the long circumradius tail (99.9th percentile 273 Mpc/h) and the 0.37% of tetrahedra extending beyond the padding. Reword to reflect the residual tail.
  3. [§5 conclusion (i) and Table 4] The conclusion says deduplication removes '10 per cent excess length from tile overlaps', but Table 4 shows the filter-only configuration has 108.44% of the reference length, an excess of ~8.4%, not 10%. Correct the number.
  4. [§4.3] The phrase 'parameter free identification of DisPerSE' is inaccurate: DisPerSE has a user-specified persistence threshold nσ and smoothing parameter, as the paper itself describes in §2.2. Rephrase as e.g. 'non-stochastic' or 'deterministic with a single significance threshold'.

Circularity Check

0 steps flagged

No significant circularity: tiling validated against an independent monolithic benchmark; connectivity compared with external theory.

full rationale

The paper's derivation chain is self-contained rather than circular. The frozen-core guarantee (§2.4, Fig. 1) is the standard Delaunay empty-circumsphere property: if a tetrahedron's circumsphere lies entirely inside a padded tile, no point outside the tile can lie inside that sphere, so the tetrahedron is valid in the global tessellation. This is a mathematical implication, not a fit. The padding width P=60 Mpc/h is calibrated from the circumradius distribution of the same catalogue, but the headline validation is an independent pipeline comparison: the tiled output is matched against a monolithic DisPerSE run on a 300 Mpc/h subvolume (§2.5.4, Table 3), and the one post-processing parameter δ=0.5 Mpc/h is shown to be stable over δ<0.7 Mpc/h (Appendix A2), so the 99.6% length / 94.7% filament recovery are not forced by construction. The connectivity slope (§3.3.4) is measured from the produced catalogue and then compared with external analytic and gas-based results (Codis et al. 2018; Santoni et al. 2024); it is not derived from them. The paper explicitly flags the finite-padding caveat in §4.2 ('to within the 0.37 per cent of tetrahedra whose circumspheres extend beyond the padding'), i.e. the monolithic reference is not the exact global complex of the full 1 Gpc/h box. That is a validation-ground-truth limitation, honestly stated, but not a circular reduction: no central number is defined in terms of the quantity it is supposed to predict, and no load-bearing step rests on a self-citation chain.

Axiom & Free-Parameter Ledger

7 free parameters · 5 axioms · 0 invented entities

No new physical entities are postulated. The method rests on standard Delaunay geometry plus the empirical assumption that a 60 h^-1 Mpc-padded 300 h^-1 Mpc run stands in for global topology. Several hand-set thresholds (P, delta, n_sigma, mass cut, cleaning parameters) shape the catalogue and connectivity slope, but none are fitted to the final scientific target (the slope).

free parameters (7)
  • Padding width P = 60 h^-1 Mpc
    Chosen from the circumradius distribution of the validation subvolume so that 99.33% of tetrahedra are captured; 30 h^-1 Mpc already gave 100% recovery (Fig. 3), so this has margin.
  • Matching tolerance delta = 0.5 h^-1 Mpc
    Single empirical parameter for deduplication and stitching; sensitivity tests show stability for delta <= 0.7 h^-1 Mpc and over-stitching at larger values (Appendix A2, Table A2).
  • Persistence threshold n_sigma = 6.5 (fiducial)
    Calibrated by critical-point/halo purity-completeness (Appendix A3); the catalogue is also produced at n_sigma = 6.0 and 7.0.
  • 20-particle mass cut = M_vir >= 3.02e10 h^-1 M_sun
    Removes poorly resolved haloes and changes the tracer density, inter-halo separation, circumradius scale, and hence padding requirements.
  • Topological cleaning thresholds (zero-length, isolated maxima, length filter) = 0.01 h^-1 Mpc, degree-1 removal, 1 h^-1 Mpc
    Hand-set from literature conventions (Malavasi et al. 2020; Galarraga-Espinosa et al. 2020); affects filament count and connectivity but not length recovery.
  • Filament merging angle and endpoint tolerance = 60 degrees, 0.5 h^-1 Mpc
    Post-processing choices that convert DisPerSE arcs into physical filaments; affect connectivity values and the fitted slope.
  • Smoothing iterations = 10
    Laplacian smoothing of stitched filaments; chosen because marginal improvement saturates below 0.3% per additional iteration.
axioms (5)
  • standard math The empty-circumsphere property characterizes Delaunay tetrahedra globally.
    Used in §2.4 and Fig. 1 to argue that a tetrahedron whose circumsphere fits inside the padded block is a valid global Delaunay tetrahedron.
  • domain assumption The 300 h^-1 Mpc monolithic run with 60 h^-1 Mpc padding represents the true global topology.
    The validation (§2.5.4) compares tiled output to this reference; if points beyond the padding would change the tessellation, the reference itself is approximate (tail circumradii reach 273 h^-1 Mpc, Table 1).
  • domain assumption DisPerSE's Morse-Smale complex on the 20-particle-cut halo catalogue defines the physical cosmic-web filaments.
    The whole analysis inherits DisPerSE's filament definition and the halo catalogue as tracer; changing the tracer density would require re-evaluating the padding and thresholds.
  • ad hoc to paper The purity/completeness ratio calibration (R ~ 1) selects the correct persistence threshold.
    Appendix A3 uses an empirical mass-threshold and R=1 criterion to justify n_sigma = 6.5; the paper itself shows the crossing shifts with halo mass cut.
  • domain assumption Codis et al. (2018) provides the theoretical mass-connectivity scaling being confirmed.
    The paper compares its power-law slope to theory/other measurements, but Codis et al. use a linear kappa-logM formula and a different topological definition, so the mapping between the two is assumed rather than derived.

pith-pipeline@v1.3.0-alltime-deepseek · 29905 in / 15719 out tokens · 135983 ms · 2026-08-02T01:02:50.934983+00:00 · methodology

0 comments
read the original abstract

Cosmic filaments are the longest structures in the Universe and the dominant element of the cosmic web, channelling matter onto clusters and shaping the environments in which galaxies form and evolve. Accurate reconstructions of this network across gigaparsec volumes are increasingly important for cosmology and galaxy evolution. However, the most commonly used topological filament finder, DisPerSE (Discrete Persistent Structures Extractor), faces a memory bottleneck: it requires a Delaunay tessellation of the full input point set, preventing application to large simulations. Naively splitting the volume fails, as different sub-volumes yield inconsistent tessellations and filament networks. We present a frozen-core method that overcomes this bottleneck while preserving the global topology. The volume is decomposed into overlapping blocks whose tessellations are filtered by a circumsphere criterion retaining only globally valid tetrahedra; a post-processing pipeline merges the tiled outputs through core filtering, deduplication, and boundary stitching. Validation against a monolithic reference on a $300\,h^{-1}\,\mathrm{Mpc}$ MDPL2 subvolume shows 99.6% total length recovery, 100% recovery of density maxima and minima, and 94.7% individual filament matching (the ${\sim}$5% of unmatched filaments are predominantly short, low-significance structures). We apply the method to the full $(1\,h^{-1}\,\mathrm{Gpc})^3$ MDPL2 box (92 million haloes), producing a gigaparsec-scale filament catalogue. As a first application, we measure the connectivity ($\kappa$) for 22,900 haloes spanning $M_{200\mathrm{c}} = 10^{12}$-$10^{15.5}\,h^{-1}\,\mathrm{M}_\odot$, finding a power-law mass-connectivity relation that extends from group to cluster scales, providing the first confirmation in an $N$-body halo catalogue that the theoretically predicted scaling holds across three decades in halo mass.

Figures

Figures reproduced from arXiv: 2607.14785 by Ankit Singh, Frazer Pearce, Gustavo Yepes, Meghan Gray.

Figure 1
Figure 1. Figure 1: Schematic illustration of the frozen-core concept in 2D. The in￾ner core region (blue, solid boundary) is surrounded by a padding layer of width P (grey, dashed boundary). Delaunay triangles (the 2D analogue of tetrahedra) in the core are classified by their circumcircles: a triangle whose circumcircle fits entirely within the padded tile (green) is frozen – guaranteed to match the global tessellation – an… view at source ↗
Figure 2
Figure 2. Figure 2: Circumsphere radius distribution and padding selection [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Boundary effects on filament detection in a 300 Mpc h −1 sub-volume without padding, compared to the fully-padded 60 Mpc h −1 reference, which reproduces the monolithic result (nσ = 6.5). Filaments are matched by centroid proximity (< 0.5 Mpc h −1 ; centroid = mean position of all sampling points). Even half the fiducial padding, 30 Mpc h −1 , already achieves 100 per cent recovery everywhere (annotated in… view at source ↗
Figure 4
Figure 4. Figure 4: Visual comparison of filament detection between single-core reference and tiled approach (nσ = 7.0, smoothing = 8, 20-particle mass cut) in a 10 Mpc h −1 -thick slice at z = 150 Mpc h −1 . Left: monolithic reference overlaid on the log-scaled halo density field (n = 1,443 filaments in slice). Centre: tiled approach (n = 1,394); dashed white lines mark tile boundaries at 100 and 200 Mpc h −1 . Right: differ… view at source ↗
Figure 5
Figure 5. Figure 5: Filament length distribution comparison between single-core (green) and tiled (red) approaches (20-particle mass cut). Left: Histogram showing near￾identical distributions. Right: Cumulative distribution confirming 99.6 per cent total length recovery. The Kolmogorov–Smirnov statistic is 0.025, indicating statistically similar distributions. 2.5.2 Stage 2: Spatial Deduplication Despite frozen-core filtering… view at source ↗
Figure 6
Figure 6. Figure 6: Unmatched filament analysis between single-core reference and tiled output (20-particle mass cut). Left: Length distribution of matched (green) vs. unmatched (red) filaments; unmatched filaments are systematically shorter (mean 4.2 Mpc h −1 vs. 6.6 Mpc h −1 ). Centre: Distance to nearest tile boundary; long unmatched filaments cluster near boundaries, while short ones are distributed throughout. Right: Joi… view at source ↗
Figure 7
Figure 7. Figure 7: Overlay of the filament network at three persistence thresholds for cluster number 6 from The Three Hundred project (Cui et al. 2018, also shown in [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Filament length distributions for the three persistence thresholds. (a) Histogram showing the count distribution on a logarithmic length axis; the total count decreases and the peak shifts to longer filaments with increasing nσ. (b) Cumulative fraction showing the broadening of the distribution toward longer filaments at higher thresholds; the x-axis is limited to ∼32 Mpc h −1 where the cumulative fraction… view at source ↗
Figure 9
Figure 9. Figure 9: (a) Length percentiles for each persistence threshold; the distribution shifts to longer lengths at higher nσ across all percentiles. (b) Count ratio relative to nσ = 6.0 as a function of filament length. Short filaments (L < 2 Mpc h −1 ) retain only ∼10 per cent of their population at nσ = 7.0, while the ratio exceeds unity for L ≳ 20 Mpc h −1 as persistence pair cancellation merges shorter arcs into long… view at source ↗
Figure 10
Figure 10. Figure 10: The filament network in the 1 Gpc MDPL2 simulation at nσ = 6.5. Top: Galaxy overdensity field (colour scale) in a 20 Mpc h −1 thick projection at z = 950 Mpc h −1 , with filaments overlaid. Coloured boxes mark regions shown in the inset panels. Bottom: Zoom into 100 Mpc h −1 regions around three clusters from The Three Hundred project (Cui et al. 2018), showing the convergence of filaments toward the most… view at source ↗
Figure 11
Figure 11. Figure 11: Connectivity illustration for three example clusters at nσ = 6.5, each in a 40 × 40 Mpc h −1 region. Orange lines: background filaments within ±10 Mpc h −1 of the cluster’s z-coordinate. Blue lines: arcs crossing the 1.5 R200 shell (dashed circle) in the post-processed catalogue. The red cross marks the cluster centre. Note that κ is measured in three dimensions, whereas each panel shows only a ±10 Mpc h … view at source ↗
Figure 12
Figure 12. Figure 12: Distribution of connectivity κ measured at 1.5 R200 for the 324 most massive clusters in MDPL2 at three persistence thresholds, after the five-step topological cleaning pipeline (including merging and 10-iteration smoothing). The mean connectivity decreases from ⟨κ⟩ = 6.0 at nσ = 6.0 to ⟨κ⟩ = 4.7 at nσ = 7.0. et al. (2023) studied filaments connected to the Coma cluster using DisPerSE applied to both SDSS… view at source ↗
Figure 13
Figure 13. Figure 13: Mass-connectivity relation for ∼22,900 haloes (M200c = 1012–1015.5 h −1 M⊙), measured on the 20-particle mass cut filament catalogue. Left: Aperture 1.5 R200. Right: Fixed aperture 1 h −1 Mpc. Large symbols show the binned means (0.25 dex bins) for the three persistence thresholds; error bars show bootstrap 1σ confidence intervals on the mean (1,000 resamples per bin). The shaded band shows the interquart… view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

72 extracted references · 1 canonical work pages

  1. [1]

    , keywords =

    Ultraviolet and optical view of galaxies in the Coma supercluster. , keywords =. doi:10.1093/mnras/sty1370 , archivePrefix =. 1805.09029 , primaryClass =

    Pith/arXiv arXiv

  2. [2]

    , keywords =

    The Environmental Dependence of the Stellar Mass - Gas Metallicity Relation in Horizon Run 5. , keywords =. doi:10.1093/mnras/stae1384 , archivePrefix =. 2404.10055 , primaryClass =

    Pith/arXiv arXiv

  3. [3]

    , keywords =

    The role of large-scale environment in shaping the stellar mass-gas metallicity relation across time. , keywords =. doi:10.1093/mnras/stag199 , archivePrefix =. 2503.12928 , primaryClass =

    arXiv

  4. [4]

    3: The constructions and statistics of 3-D Voronoi tessellations

    Fragmenting the Universe. 3: The constructions and statistics of 3-D Voronoi tessellations. , keywords =

  5. [5]

    , keywords =

    Multiscale phenomenology of the cosmic web. , keywords =. doi:10.1111/j.1365-2966.2010.17263.x , archivePrefix =. 1007.0742 , primaryClass =

    arXiv 2010

  6. [7]

    Illustrations

    The persistent cosmic web and its filamentary structure - II. Illustrations. , keywords =. doi:10.1111/j.1365-2966.2011.18395.x , archivePrefix =. 1009.4014 , primaryClass =

    arXiv 2011

  7. [8]

    , keywords =

    Galaxy And Mass Assembly (GAMA): stellar mass growth of spiral galaxies in the cosmic web. , keywords =. doi:10.1093/mnras/stw134 , archivePrefix =. 1601.03391 , primaryClass =

    Pith/arXiv arXiv

  8. [9]

    , keywords =

    From voids to filaments: environmental transformations of galaxies in the SDSS. , keywords =. doi:10.1051/0004-6361/201730526 , archivePrefix =. 1703.04338 , primaryClass =

    Pith/arXiv arXiv

  9. [10]

    , keywords =

    Study of galaxies on large-scale filaments in simulations. , keywords =. doi:10.1093/mnras/staa1913 , archivePrefix =. 2007.01149 , primaryClass =

    Pith/arXiv arXiv 2007

  10. [11]

    , keywords =

    The Statistics of Peaks of Gaussian Random Fields. , keywords =. doi:10.1086/164143 , adsurl =

    doi:10.1086/164143

  11. [12]

    , keywords =

    The ROCKSTAR Phase-Space Temporal Halo Finder and the Velocity Offsets of Cluster Cores. , keywords =. doi:10.1088/0004-637X/762/2/109 , archivePrefix =. 1110.4372 , primaryClass =

    Pith/arXiv arXiv

  12. [13]

    1996 , url =

    J Richard Bond and Lev Kofmant and Dmitry Pogosyan , title =. 1996 , url =. doi:https://doi.org/10.1038/380603a0 , journal =

    doi:10.1038/380603a0 1996

  13. [14]

    How galaxy properties vary with filament proximity in the SIMBA simulations , url =

    Teodora-Elena Bulichi and Romeel Dave and Katarina Kraljic , month =. How galaxy properties vary with filament proximity in the SIMBA simulations , url =. doi:https://doi.org/10.48550/arXiv.2309.03282 , journal =

    Pith/arXiv arXiv doi:10.48550/arxiv.2309.03282

  14. [15]

    , keywords =

    NEXUS: tracing the cosmic web connection. , keywords =. doi:10.1093/mnras/sts416 , archivePrefix =. 1209.2043 , primaryClass =

    Pith/arXiv arXiv 2043

  15. [16]

    , keywords =

    Evolution of the cosmic web. , keywords =. doi:10.1093/mnras/stu768 , archivePrefix =. 1401.7866 , primaryClass =

    Pith/arXiv arXiv

  16. [17]

    , keywords =

    Where Are the Baryons?. , keywords =. doi:10.1086/306949 , archivePrefix =. astro-ph/9806281 , primaryClass =

    Pith/arXiv arXiv

  17. [18]

    , keywords =

    Detecting effects of filaments on galaxy properties in the Sloan Digital Sky Survey III. , keywords =. doi:10.1093/mnras/stw3127 , archivePrefix =. 1509.06376 , primaryClass =

    Pith/arXiv arXiv

  18. [19]

    , keywords =

    On the connectivity of the cosmic web: theory and implications for cosmology and galaxy formation. , keywords =. doi:10.1093/mnras/sty1643 , archivePrefix =. 1803.11477 , primaryClass =

    Pith/arXiv arXiv

  19. [20]

    , keywords =

    The localization of galaxy groups in close proximity to galaxy clusters using cosmic web nodes. , keywords =. doi:10.1093/mnras/stad3205 , archivePrefix =. 2310.11268 , primaryClass =

    Pith/arXiv arXiv

  20. [21]

    , keywords =

    The Three Hundred project: a large catalogue of theoretically modelled galaxy clusters for cosmological and astrophysical applications. , keywords =. doi:10.1093/mnras/sty2111 , archivePrefix =. 1809.04622 , primaryClass =

    Pith/arXiv arXiv

  21. [22]

    , keywords =

    Group connectivity in COSMOS: a tracer of mass assembly history. , keywords =. doi:10.1093/mnras/stz2490 , archivePrefix =. 1904.11859 , primaryClass =

    Pith/arXiv arXiv 1904

  22. [23]

    , keywords =

    Spectroscopic Study of Star-forming Galaxies in Filaments and the Field at z -0.5ex 0.5: Evidence for Environmental Dependence of Electron Density. , keywords =. doi:10.1088/0004-637X/814/2/84 , archivePrefix =. 1510.05009 , primaryClass =

    Pith/arXiv arXiv

  23. [24]

    , keywords =

    Cold streams in early massive hot haloes as the main mode of galaxy formation. , keywords =. doi:10.1038/nature07648 , archivePrefix =. 0808.0553 , primaryClass =

    Pith/arXiv arXiv

  24. [25]

    A SLICE OF THE UNIVERSE 1 , volume =

    Valérie de Lapparent and Margaret J Geller and John P Huchra , doi =. A SLICE OF THE UNIVERSE 1 , volume =. The Astrophysical Journal , keywords =

  25. [26]

    The role of the cosmic web in the scatter of the galaxy stellar mass - gas metallicity relation , url =

    Callumn Donnan and Rita Tojeiro and Katarina Kraljic , journal =. The role of the cosmic web in the scatter of the galaxy stellar mass - gas metallicity relation , url =. doi:https://doi.org/10.1038/s41550-022-01619-w , month =

    doi:10.1038/s41550-022-01619-w

  26. [27]

    , keywords =

    Galaxy morphology in rich clusters: implications for the formation and evolution of galaxies. , keywords =. doi:10.1086/157753 , adsurl =

    doi:10.1086/157753

  27. [28]

    Contemporary Mathematics , year = 2008, volume =

    Persistent homology --- a survey. Contemporary Mathematics , year = 2008, volume =

    2008

  28. [29]

    , keywords =

    Populations of filaments from the distribution of galaxies in numerical simulations. , keywords =. doi:10.1051/0004-6361/202037986 , archivePrefix =. 2003.09697 , primaryClass =

    Pith/arXiv arXiv 2003

  29. [30]

    , keywords =

    Distinguish satisfactory and unsatisfactory dark matter models with the cosmic web. , keywords =. doi:10.1051/0004-6361/202452238 , archivePrefix =. 2402.04837 , primaryClass =

    Pith/arXiv arXiv

  30. [31]

    , keywords =

    Properties of gas phases around cosmic filaments at z = 0 in the IllustrisTNG simulation. , keywords =. doi:10.1051/0004-6361/202039781 , archivePrefix =. 2010.15139 , primaryClass =

    Pith/arXiv arXiv 2010

  31. [32]

    , keywords =

    Relative distribution of dark matter, gas, and stars around cosmic filaments in the IllustrisTNG simulation. , keywords =. doi:10.1051/0004-6361/202141974 , archivePrefix =. 2109.06198 , primaryClass =

    Pith/arXiv arXiv

  32. [33]

    , keywords =

    Evolution of cosmic filaments in the MTNG simulation. , keywords =. doi:10.1051/0004-6361/202347982 , archivePrefix =. 2309.08659 , primaryClass =

    Pith/arXiv arXiv

  33. [34]

    1989 , doi =

    Margaret J Geller and John P Huchra , title =. 1989 , doi =

    1989

  34. [35]

    Gouin and T

    C. Gouin and T. Bonnaire and N. Aghanim , doi =. Shape and connectivity of groups and clusters: Effect of the dynamical state and accretion history , volume =. Astronomy and Astrophysics , keywords =. 2101.04686 , archivePrefix =

    Pith/arXiv arXiv

  35. [36]

    , keywords =

    The Evolving Effect of Cosmic Web Environment on Galaxy Quenching. , keywords =. doi:10.3847/1538-4357/acd11c , archivePrefix =. 2303.08088 , primaryClass =

    Pith/arXiv arXiv

  36. [37]

    , keywords =

    The effect of cosmic web filaments on galaxy properties in the RESOLVE and ECO surveys. , keywords =. doi:10.1093/mnras/stae066 , archivePrefix =. 2401.09114 , primaryClass =

    Pith/arXiv arXiv

  37. [38]

    , keywords =

    How do galaxies get their gas?. , keywords =. doi:10.1111/j.1365-2966.2005.09451.x , archivePrefix =. astro-ph/0407095 , primaryClass =

    arXiv 2005

  38. [39]

    , keywords =

    MultiDark simulations: the story of dark matter halo concentrations and density profiles. , keywords =. doi:10.1093/mnras/stw248 , archivePrefix =. 1411.4001 , primaryClass =

    Pith/arXiv arXiv

  39. [40]

    , keywords =

    Galaxy evolution in the metric of the cosmic web. , keywords =. doi:10.1093/mnras/stx2638 , archivePrefix =. 1710.02676 , primaryClass =

    Pith/arXiv arXiv

  40. [41]

    , keywords =

    COSMOS2015 photometric redshifts probe the impact of filaments on galaxy properties. , keywords =. doi:10.1093/mnras/stx3055 , archivePrefix =. 1702.08810 , primaryClass =

    Pith/arXiv arXiv

  41. [42]

    , keywords =

    Tracing the cosmic web. , keywords =. doi:10.1093/mnras/stx1976 , archivePrefix =. 1705.03021 , primaryClass =

    Pith/arXiv arXiv

  42. [43]

    Galaxy segregation on the cosmic web from PDR-2

    The VIMOS Public Extragalactic Redshift Survey. Galaxy segregation on the cosmic web from PDR-2. , keywords =. doi:10.1093/mnras/stw2864 , archivePrefix =. 1611.07045 , primaryClass =

    Pith/arXiv arXiv

  43. [44]

    , keywords =

    Like a spider in its web: a study of the large-scale structure around the Coma cluster. , keywords =. doi:10.1051/0004-6361/201936629 , archivePrefix =. 1910.11879 , primaryClass =

    Pith/arXiv arXiv 1910

  44. [45]

    , keywords =

    The Effect of Filaments and Tendrils on the H I Content of Galaxies. , keywords =. doi:10.3847/1538-4357/aaa1e8 , archivePrefix =. 1712.05045 , primaryClass =

    Pith/arXiv arXiv

  45. [46]

    and Boots, B

    Okabe, A. and Boots, B. and Sugihara, K. and Chiu, S. N. , title =

  46. [47]

    , keywords =

    The effect of cosmic web filaments on galaxy evolution. , keywords =. doi:10.1093/mnras/stae2142 , archivePrefix =. 2409.09028 , primaryClass =

    Pith/arXiv arXiv

  47. [48]

    , keywords =

    Mass and Environment as Drivers of Galaxy Evolution in SDSS and zCOSMOS and the Origin of the Schechter Function. , keywords =. doi:10.1088/0004-637X/721/1/193 , archivePrefix =. 1003.4747 , primaryClass =

    Pith/arXiv arXiv

  48. [49]

    Planck 2013 results. XVI. Cosmological parameters. , year = 2014, month = nov, volume =. doi:10.1051/0004-6361/201321591 , archivePrefix =. 1303.5076 , primaryClass =

    Pith/arXiv arXiv 2013

  49. [50]

    Astronomische Nachrichten , keywords =

    The MultiDark Database: Release of the Bolshoi and MultiDark cosmological simulations. Astronomische Nachrichten , keywords =. doi:10.1002/asna.201211900 , archivePrefix =. 1109.0003 , primaryClass =

    Pith/arXiv arXiv

  50. [51]

    , keywords =

    THE THREE HUNDRED project: Estimating the dependence of gas filaments on the mass of galaxy clusters. , keywords =. doi:10.1051/0004-6361/202450895 , archivePrefix =. 2405.17239 , primaryClass =

    Pith/arXiv arXiv

  51. [52]

    Sarron and C

    F. Sarron and C. Adami and F. Durret and C. Laigle , doi =. Pre-processing of galaxies in cosmic filaments around AMASCFI clusters in the CFHTLS , volume =. Astronomy and Astrophysics , keywords =

  52. [53]

    , keywords =

    Continuous fields and discrete samples: reconstruction through Delaunay tessellations. , keywords =

  53. [54]

    Beyond halo mass: Quenching galaxy mass assembly at the edge of filaments , volume =

    Hyunmi Song and Clotilde Laigle and Ho Seong Hwang and Julien Devriendt and Yohan Dubois and Katarina Kraljic and Christophe Pichon and Adrianne Slyz and Rory Smith , doi =. Beyond halo mass: Quenching galaxy mass assembly at the edge of filaments , volume =. Monthly Notices of the Royal Astronomical Society , keywords =

  54. [55]

    , keywords =

    Detecting filamentary pattern in the cosmic web: a catalogue of filaments for the SDSS. , keywords =. doi:10.1093/mnras/stt2454 , archivePrefix =. 1308.2533 , primaryClass =

    Pith/arXiv arXiv

  55. [56]

    , keywords =

    An unbiased study of the association of large-scale structure with AGN and galaxy evolution. , keywords =. doi:10.1093/mnras/stz1399 , archivePrefix =. 1905.08942 , primaryClass =

    Pith/arXiv arXiv 1905

  56. [57]

    Fragmentation of a homogeneous medium under the action of gravitation

    Ya B Zel'dovich , issue =. Fragmentation of a homogeneous medium under the action of gravitation. , volume =. doi:https://doi.org/10.1007/BF01007263 , journal =

    work page doi:10.1007/bf01007263

  57. [58]

    , keywords =

    Baryons in the Warm-Hot Intergalactic Medium. , keywords =. doi:10.1086/320548 , archivePrefix =. astro-ph/0007217 , adsurl =

    Pith/arXiv arXiv

  58. [59]

    , keywords =

    The effects of the cosmic web on galaxy evolution. , keywords =. doi:10.1093/mnras/staa1083 , archivePrefix =. 2004.08408 , adsurl =

    Pith/arXiv arXiv 2004

  59. [60]

    , keywords =

    Cosmic filaments in galaxy cluster outskirts: quantifying finding filaments in redshift space. , keywords =. doi:10.1093/mnras/stab567 , archivePrefix =. 2102.12500 , adsurl =

    Pith/arXiv arXiv

  60. [61]

    , keywords =

    Topological bias: how haloes trace structural patterns in the cosmic web. , keywords =. doi:10.1093/mnras/stae801 , archivePrefix =. 2206.14655 , adsurl =

    Pith/arXiv arXiv

  61. [62]

    The cosmic web around the Coma cluster from constrained cosmological simulations. I. Filaments connected to Coma at z = 0. , keywords =. doi:10.1051/0004-6361/202245777 , archivePrefix =. 2306.03124 , adsurl =

    Pith/arXiv arXiv

  62. [63]

    , year = 2023, volume =

    The MillenniumTNG Project: the hydrodynamical full physics simulations, their calibration and validation. , year = 2023, volume =. doi:10.1093/mnras/stad2027 , archivePrefix =. 2210.10060 , primaryClass =

    Pith/arXiv arXiv 2023

  63. [64]

    , year = 2023, volume =

    The FLAMINGO project: cosmological hydrodynamical simulations for large-scale structure and galaxy cluster surveys. , year = 2023, volume =. doi:10.1093/mnras/stad2419 , archivePrefix =. 2306.04024 , primaryClass =

    Pith/arXiv arXiv 2023

  64. [65]

    Euclid. V. The Flagship galaxy mock catalogue. , year = 2025, doi =

    2025

  65. [66]

    arXiv e-prints , keywords =

    Large Scale Structure and the Cosmic Web. arXiv e-prints , keywords =. doi:10.48550/arXiv.2503.21759 , archivePrefix =. 2503.21759 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2503.21759

  66. [67]

    , keywords =

    Statistical Properties of X-Ray Clusters: Analytic and Numerical Comparisons. , keywords =. doi:10.1086/305262 , archivePrefix =. astro-ph/9710107 , adsurl =

    Pith/arXiv arXiv

  67. [68]

    Intercluster filaments in a

    Colberg, J. Intercluster filaments in a. Monthly Notices of the Royal Astronomical Society , volume =. 2005 , month = may, doi =

    2005

  68. [69]

    Cohn, J. D. , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2022 , month = jun, doi =. 2108.02292 , archivePrefix=

    Pith/arXiv arXiv 2022

  69. [70]

    Monthly Notices of the Royal Astronomical Society , volume =

    Zhang, Youcai and Guo, Hong and Yang, Xiaohu and Wang, Peng , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2024 , month = sep, doi =. 2408.03083 , archivePrefix=

    Pith/arXiv arXiv 2024

  70. [71]

    arXiv e-prints , keywords =

    Evolution of submillimeter galaxies across cosmic-web environments. arXiv e-prints , keywords =

  71. [72]

    The role of cosmic connectivity in shaping galaxy clusters

    Euclid Quick Data Release (Q1). The role of cosmic connectivity in shaping galaxy clusters. arXiv e-prints , keywords =

  72. [73]

    Galaxy shapes and alignments in the cosmic web

    Euclid Quick Data Release (Q1). Galaxy shapes and alignments in the cosmic web. arXiv e-prints , keywords =