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REVIEW 3 major objections 5 minor 107 references

Filaments are the primary environment sustaining the large-scale conformity signal once former satellites are removed.

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2026-08-01 04:21 UTC pith:CWWKF7AE

load-bearing objection New environmental decomposition shows filaments host residual conformity in both models, but the claim that they are primary contributors is undercut by the paper's own removal test. the 3 major comments →

arxiv 2607.22838 v1 pith:CWWKF7AE submitted 2026-07-24 astro-ph.GA

The role of filaments in the large-scale conformity signal

Daniela Palma , Ivan Lacerna , Noelia P\'erez , Luis Pereyra , Antonio D. Montero-Dorta , Constanza A. Soto-Su\'arez , Laerte Sodr\'e Jr. , M. Celeste Artale
show 3 more authors
Amrutha Belwadi Facundo Rodriguez Nelvy Choque-Challapa
This is my paper
classification astro-ph.GA
keywords large-scale conformitytwo-halo conformitycosmic web filamentslow-mass central galaxiesenvironmental quenchinggalaxy formation simulationsDisPerSE filament findinggalaxy assembly bias
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.

This paper asks what physical environment generates the two-halo conformity signal—the correlation between the star-formation state of a low-mass central galaxy and that of galaxies several megaparsecs away—after previously accreted 'former satellite' galaxies are removed. Using two independent galaxy-formation models on cosmological simulations, the authors classify low-mass central galaxies into cosmic-web environments: group outskirts, cluster outskirts, filaments, filament outskirts, and everything else. They find that, in the semi-analytic model, galaxies embedded in filaments and their immediate outskirts reproduce the full shape and amplitude of the residual conformity signal, dominating over contributions from group and cluster outskirts; in the hydrodynamic model, filament residents produce a weaker but coherent signal once former satellites are excluded. The signal is insensitive to filament thickness and overlap, but is stronger in high-linear-density, short, and massive filaments, and is amplified near interacting massive systems. The paper concludes that filamentary regions and tidal influences, not pre-processing alone, sustain the large-scale conformity signal.

Core claim

The paper's central claim is that the large-scale conformity signal left after removing former satellite galaxies is traced by cosmic-web filaments rather than by the near-virial environment of groups and clusters. In the semi-analytic model, galaxies within about 1 h^-1 Mpc of a filament spine, or in the 1-2 h^-1 Mpc 'filament outskirts,' reproduce the global conformity curve—reaching roughly 99% and 93% of the total amplitude at small separations and exceeding it at intermediate separations—whereas group and cluster outskirts contribute only within roughly 1.5-2 h^-1 Mpc. In the hydrodynamic simulation, the same filamentary environments give the only statistically significant contribution

What carries the argument

DisPerSE, a discrete-Morse-theory filament finder, reconstructs the cosmic web from galaxy positions and assigns each low-mass central galaxy to one of five environments by perpendicular distance to filament spines (within 1 h^-1 Mpc for filaments, 1-2 h^-1 Mpc for filament outskirts, and 1-3 virial radii for group and cluster outskirts). The conformity measure is the difference between the mean quenched fraction of neighbor galaxies around quenched versus star-forming central galaxies as a function of separation, with bootstrap resampling for uncertainties. The key work of this machinery is to partition the residual signal by environment, allowing a direct shape-and-amplitude comparison to

Load-bearing premise

The load-bearing premise is that the DisPerSE classification of galaxies as filament residents—using different tracer populations and persistence thresholds in the two models, and a fixed 1 h^-1 Mpc perpendicular distance—correctly captures the physically relevant filamentary environment; if that classification is biased, the dominance of filaments could be a selection artifact rather than a physical effect.

What would settle it

Run the entire environment classification with a single tracer choice (for instance, all dark-matter halos above the same mass in both simulations) and a single persistence threshold, and vary the perpendicular distance used to assign galaxies to filaments from 0.5 to 2 h^-1 Mpc. If the filamentary population no longer reproduces the global conformity curve, or if the amplitude difference between the two models is simply the difference in filament fractions, the paper's attribution to filaments would be a classification artifact. An observational check is to measure the quenched-fraction diffe

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

If this is right

  • Removing former satellites does not erase conformity: the residual signal lives in filaments and their outskirts, so pre-processing and backsplash are not the whole story.
  • Group and cluster outskirts contribute only at separations below roughly 1.5-2 h^-1 Mpc; beyond that, filamentary regions are the main carriers of the signal.
  • Filament-related conformity is generic: it appears in both a semi-analytic and a hydrodynamic model despite substantial differences in prescriptions and resolution.
  • The signal is insensitive to filament thickness and overlap, but its amplitude tracks filament density, length, and mass, suggesting denser filaments act more strongly.
  • Galaxies near interacting massive systems show amplified conformity up to about 4 h^-1 Mpc, pointing to tidal fields as an enhancing mechanism.

Where Pith is reading between the lines

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

  • If the filament association is physical, low-mass central galaxies inside filaments should show correlated star-formation histories with their neighbors in observed surveys; measuring the same quenched-fraction difference inside versus outside filaments would be a direct observational test.
  • The denser-shorter-more-massive filament dependence predicts an assembly-bias gradient along filaments: early-forming halos with stalled accretion should preferentially populate dense filaments, tying the conformity signal to halo assembly history.
  • A controlled experiment using identical tracer populations and persistence thresholds across both simulations would isolate whether the model difference in filamentary fractions is driving the amplitude difference, rather than a physical effect.
  • If tidal amplification near interacting massive systems is real, the signal should strengthen with the mass ratio and proximity of the interacting pair and should appear as an excess of quenched galaxies on the line connecting two clusters.

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 / 5 minor

Summary. The paper investigates the origin of the large-scale (two-halo) conformity signal for low-mass central galaxies after excluding former satellites, using the hydrodynamical simulation IllustrisTNG300 and the semi-analytic model MDPL2-SAG. The authors classify central galaxies with DisPerSE into group outskirts, cluster outskirts, filaments, filament outskirts, and other environments, and measure the quenched-fraction difference Δf_Q around quenched vs star-forming centrals in each environment. They report that in SAG, galaxies in filamentary regions closely reproduce the shape and amplitude of the total signal, while group/cluster outskirts contribute mainly at small separations; in TNG300 the filamentary signal is weaker but apparently coherent. They also test robustness to filament thickness and overlap, split filaments by length, linear density, and mass, and examine the effect of nearby merger-candidate massive systems.

Significance. The topic is timely: connecting the large-scale conformity signal to the cosmic web could provide a physical mechanism beyond backsplash galaxies and assembly bias. The analysis benefits from using two complementary models, bootstrap error estimates, and robustness checks on filament thickness and overlap. No parameters are fitted to reproduce the signal, and the interpretation is presented as a decomposition of a measured statistic. If the conclusions were fully supported, the paper would be a useful step toward understanding the environmental origin of conformity. However, as detailed below, the central claim about the 'primary' role of filaments is not supported by the paper's own removal test and population fractions, so the significance is currently qualified by a load-bearing overstatement.

major comments (3)
  1. [Abstract; Sect. 4.1; Appendix D] The statement that filamentary galaxies are 'primary contributors' to the large-scale conformity signal in SAG is contradicted by the removal test in Fig. D.1 and by the sample fractions in Table 2. In SAG, galaxies in filaments plus filament outskirts comprise only ~5–6% of the full sample (e.g., 5010/69130 quenched and 352438/6174531 star-forming centrals). For a weighted average, the contribution of a subpopulation to Δf_Q is approximately (N_env/N_tot)Δf_env, so with Δf_fil ≈ Δf_tot the expected removal effect is only a few percent. Appendix D indeed finds 'negligible changes'. The paper conflates the per-environment signal amplitude with the contribution to the total signal. I request a quantitative decomposition — for example, computing Δf_total − Δf_total_without_env for each environment — and a revision of the abstract, Sect. 4.1, and the Conclusions to state that filaments host
  2. [Sect. 6 vs Sect. 3.1] The robustness claim that the connection between filamentary environments and the conformity signal is 'not driven by a particular choice of filament definition' is too strong, because only the filament thickness (1 vs 0.5 h−1 Mpc) and overlap assignment were varied. The DisPerSE tracer population and persistence threshold, which differ between the two models (Section 3.1: Mr<−21 with 2σ in SAG vs M*>10^9 M⊙ with 3σ in TNG300), were not varied within either model. The cross-model consistency is suggestive, but it does not constitute a controlled test of the filament definition. Please either add such a variation or soften the claim accordingly.
  3. [Sect. 4.1, Fig. 2 (right panels)] The claim that in TNG300 filamentary regions provide the 'only statistically significant contribution' should be qualified by the limited sample size. Table 2 lists only 427 quenched and 4019 star-forming centrals in filaments (and 452/4371 in filament outskirts), and the analysis is restricted to |Δf_Q| ≳ 1σ and to r < 4 h−1 Mpc. With these numbers the detection is marginal. Please state the significance (e.g., 2σ or 3σ) of the filamentary signal at each radial bin, and avoid language implying a robust detection if the signal is only at the ~1–2σ level.
minor comments (5)
  1. [Sect. 3.2, Eq. (1)] Please clarify in the text around Eq. (1) that the neighboring galaxies are selected with stellar masses above 10^9 h−1 M⊙, and specify whether the same threshold is used for both simulations.
  2. [Sect. 6] Typo: 'analizing' should be 'analyzing'.
  3. [Appendix F] This appendix appears to use all low-mass central galaxies in TNG300, including former satellites, whereas the main analysis excludes them. If so, please state explicitly that this is a robustness test and note any differences in interpretation.
  4. [Sect. 3.1, footnote 2] The sentence 'We tested the cut: sSFR∼10−11 yr−1' should specify the units (presumably h yr−1) and explain more clearly why this alternative cut was not adopted, given that it yields a reduced quenched sample in TNG300.
  5. [Fig. 2 caption and Sect. 4.1 text] The text repeatedly refers to the 'contribution' of each environment when the plotted quantity is actually the per-environment Δf_Q. Consider renaming the y-axis label or adding a clarifying sentence to distinguish the per-environment signal from the contribution to the global weighted average.

Circularity Check

0 steps flagged

No significant circularity: measurements are direct; the abstract's 'primary contributors' wording is an interpretation issue, not a derivation-from-inputs circularity.

full rationale

The paper does not derive its central result from a parameter fitted to that result. The conformity signal is measured directly as Delta f_Q = f_Q^Q - f_Q^SF from the SAG and TNG300 galaxy catalogs, and the cosmic-web environments are assigned with the fixed DisPerSE thresholds and choices taken from Galarraga-Espinosa et al. (2020, 2024). No parameter is fitted to reproduce the total signal, and the per-environment curves in Fig. 2 are independent conditional measurements rather than quantities forced by construction. The self-citations to Palma et al. (2025), Lacerna et al. (2022), and Lacerna et al. (2025) are continuations of previous work used for sample definition, comparison of the total signal, and a discussion-level interpretation; they are not invoked as an external uniqueness theorem or as an ansatz that smuggles in the conclusion. The internal tension between the abstract's 'primary contributors' language and Appendix D's removal test (negligible change after removing ~5% of galaxies in SAG) is a real quantitative concern about how 'contribution' is being interpreted, but it is not circular: the per-environment signal is not the same object as the population's actual weighted contribution to the total signal, and the paper never equates the two by definition. Thus, under the stated rules requiring a specific reduction to inputs to flag circularity, no circular step is present.

Axiom & Free-Parameter Ledger

5 free parameters · 4 axioms · 0 invented entities

The central claim rests on the fidelity of the two simulation models, the DisPerSE-based environment classification, and the chosen thresholds (filament thickness, sSFR cut, persistence). None of these are fitted to the conformity signal; they are carried over from prior literature. The paper tests robustness to filament thickness and overlap, but not to tracer choice or persistence threshold.

free parameters (5)
  • Filament thickness (perpendicular distance) = 1 h^-1 Mpc (tested 0.5 h^-1 Mpc)
    Defines galaxies in filaments; adopted from Galárraga-Espinosa et al. (2023b); robustness test confirms no significant change.
  • sSFR quenched cut = 10^-10.5 h yr^-1
    Adopted from Cora et al. (2018); used to classify star-forming vs quenched; alternative cut tested in footnote 2.
  • DisPerSE persistence threshold = 2σ (SAG), 3σ (TNG300)
    Adopted from Galárraga-Espinosa et al. (2020, 2024); not varied across models, though tracer populations differ.
  • Group/cluster mass threshold = 10^14 M_sun
    Boundary between group and cluster outskirts; chosen from Galárraga-Espinosa et al. (2023b); not varied.
  • Merger candidate separation criteria = d <= r1+r2; near <0.1 h^-1 Mpc vs 2-3 h^-1 Mpc
    Defines interacting massive systems in Appendix G; chosen to test tidal effect.
axioms (4)
  • domain assumption Simulation catalogs (TNG300, MDPL2-SAG) provide galaxy and halo properties accurate enough for this analysis.
    The paper relies on these models' subgrid physics and resolution (Sect. 2).
  • domain assumption DisPerSE, with DTFE density field and topological persistence, correctly identifies the cosmic-web filaments from tracer galaxies.
    Environment classification depends entirely on this algorithm (Sect. 3.1); no independent validation within the paper.
  • domain assumption The quenched fraction difference Δf_Q is a valid and sufficiently sensitive measure of large-scale conformity.
    Used in all previous conformity studies; the paper adopts it without re-derivation (Sect. 3.2).
  • domain assumption The removal of former satellites is complete and the remaining centrals are uncontaminated.
    The paper traces back progenitor histories to classify former satellites; errors in this classification would affect the residual signal (Sect. 3.1, 2).

pith-pipeline@v1.3.0-alltime-deepseek · 25477 in / 9039 out tokens · 81280 ms · 2026-08-01T04:21:08.978413+00:00 · methodology

0 comments
read the original abstract

We investigate the large-scale conformity signal and its connection with the large-scale structure, focusing on low-mass central galaxies, after excluding galaxies that were satellites in the past. We measure the signal across different environments identified with the DisPerSE algorithm, including group outskirts, cluster outskirts, filaments, filament outskirts, and other environments (voids and walls) in order to assess how each population contributes to the large-scale conformity signal. We use the galaxy catalogs from the IllustrisTNG300 simulation and the semi-analytic model MDPL2-SAG. In SAG, galaxies embedded in filamentary regions emerge as the primary contributors to the large-scale conformity signal, closely reproducing its overall shape and amplitude. In TNG300, galaxies located in filamentary regions also exhibit a coherent, albeit weaker, conformity signal once galaxies that were satellites in the past are excluded. We also examine whether the signal depends on the adopted filament definition. We find no substantial differences when varying the filament thickness or considering galaxies in overlapping regions. Instead, the signal remains strong and largely insensitive to these differences. We then investigate the dependence of the conformity signal on filament linear density, length, and mass. The signal is enhanced in high-linear density, short, and high-mass filaments, but remains present in low-linear density, long, and low-mass filaments, although with a slightly lower amplitude. Finally, we find that low-mass central galaxies located in close proximity to interacting massive systems show an amplified conformity signal extending up to 4 Mpc/h. Overall, our results indicate that filamentary regions, and the tidal forces from neighboring massive systems play a fundamental role in shaping the large-scale conformity signal.

Figures

Figures reproduced from arXiv: 2607.22838 by Amrutha Belwadi, Antonio D. Montero-Dorta, Constanza A. Soto-Su\'arez, Daniela Palma, Facundo Rodriguez, Ivan Lacerna, Laerte Sodr\'e Jr., Luis Pereyra, M. Celeste Artale, Nelvy Choque-Challapa, Noelia P\'erez.

Figure 1
Figure 1. Figure 1: Left panels: Distribution of low-mass central galaxies with stellar masses in the range 9 [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Conformity signal for all low-mass central galaxies in each model after removing backsplash objects (black solid line), [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 4
Figure 4. Figure 4: Conformity signal, [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 3
Figure 3. Figure 3: shows the signal produced by low-mass central galaxies in SAG located in long (solid line) vs short (dashed line) filaments, and [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 7
Figure 7. Figure 7: Probability distribution of M200 for low-mass central galaxies across different environments. The panels and colors are designed in the same way as in [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗
Figure 5
Figure 5. Figure 5: Probability distribution of gas mass for low-mass cen [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Probability distribution of sSFR for low-mass central [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗

discussion (0)

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Reference graph

Works this paper leans on

107 extracted references · 6 canonical work pages

  1. [1]

    , keywords =

    The evolution of low-mass central galaxies in the vicinity of massive structures and its impact on the two-halo conformity. , keywords =. doi:10.1051/0004-6361/202450976 , archivePrefix =. 2406.12977 , primaryClass =

    Pith/arXiv arXiv

  2. [2]

    Flows around galaxies. I. The dependence of galaxy connectivity on cosmic environments and effects on the star formation rate. , keywords =. doi:10.1051/0004-6361/202244935 , archivePrefix =. 2209.05495 , primaryClass =

    Pith/arXiv arXiv

  3. [3]

    , keywords =

    Pre- and post-processing of cluster galaxies out to 5 R _ 200 : the extreme case of A2670. , keywords =. doi:10.1093/mnras/stad3957 , archivePrefix =. 2401.06973 , primaryClass =

    Pith/arXiv arXiv

  4. [4]

    , keywords =

    Pre-Processing of Galaxies before Entering a Cluster. , keywords =. doi:10.1093/pasj/56.1.29 , archivePrefix =. astro-ph/0311193 , primaryClass =

    Pith/arXiv arXiv

  5. [5]

    , keywords =

    Galaxy evolution in groups and clusters: satellite star formation histories and quenching time-scales in a hierarchical Universe. , keywords =. doi:10.1093/mnras/stt469 , archivePrefix =. 1206.3571 , primaryClass =

    Pith/arXiv arXiv

  6. [6]

    , keywords =

    LoCuSS: The Slow Quenching of Star Formation in Cluster Galaxies and the Need for Pre-processing. , keywords =. doi:10.1088/0004-637X/806/1/101 , archivePrefix =. 1504.05604 , primaryClass =

    Pith/arXiv arXiv

  7. [7]

    , keywords =

    Tracing the quenching history of cluster galaxies in the EAGLE simulation. , keywords =. doi:10.1093/mnras/stz1745 , archivePrefix =. 1812.08802 , primaryClass =

    Pith/arXiv arXiv

  8. [8]

    , keywords =

    The Three Hundred Project: Connection between star formation quenching and dynamical evolution in and around simulated galaxy clusters. , keywords =. doi:10.1093/mnras/stac3209 , archivePrefix =. 2211.04485 , primaryClass =

    Pith/arXiv arXiv

  9. [9]

    , keywords =

    Local versus global environment: the suppression of star formation in the vicinity of galaxy clusters. , keywords =. doi:10.1093/mnras/stae1403 , archivePrefix =. 2406.02196 , primaryClass =

    Pith/arXiv arXiv

  10. [10]

    The LOFAR Two-metre Sky Survey. V. Second data release. , keywords =. doi:10.1051/0004-6361/202142484 , archivePrefix =. 2202.11733 , primaryClass =

    Pith/arXiv arXiv

  11. [11]

    , keywords =

    The 16th Data Release of the Sloan Digital Sky Surveys: First Release from the APOGEE-2 Southern Survey and Full Release of eBOSS Spectra. , keywords =. doi:10.3847/1538-4365/ab929e , archivePrefix =. 1912.02905 , primaryClass =

    arXiv 1912

  12. [12]

    , keywords =

    The physical properties of star-forming galaxies in the low-redshift Universe. , keywords =. doi:10.1111/j.1365-2966.2004.07881.x , archivePrefix =. astro-ph/0311060 , primaryClass =

    arXiv 2004

  13. [13]

    , keywords =

    The Wide-field Infrared Survey Explorer (WISE): Mission Description and Initial On-orbit Performance. , keywords =. doi:10.1088/0004-6256/140/6/1868 , archivePrefix =. 1008.0031 , primaryClass =

    Pith/arXiv arXiv

  14. [14]

    Star formation quenching in the infall region around galaxy clusters

    Salerno, Juan Manuel and Muriel, Hern. Star formation quenching in the infall region around galaxy clusters. Monthly Notices of the Royal Astronomical Society , volume =. 2022 , month =. doi:10.1093/mnras/stac2980 , url =

    work page doi:10.1093/mnras/stac2980 2022

  15. [15]

    , keywords =

    First results from the IllustrisTNG simulations: a tale of two elements - chemical evolution of magnesium and europium. , keywords =. doi:10.1093/mnras/sty618 , archivePrefix =. 1707.03401 , primaryClass =

    Pith/arXiv arXiv

  16. [16]

    , keywords =

    First results from the IllustrisTNG simulations: the galaxy colour bimodality. , keywords =. doi:10.1093/mnras/stx3040 , archivePrefix =. 1707.03395 , primaryClass =

    Pith/arXiv arXiv

  17. [17]

    , keywords =

    First results from the IllustrisTNG simulations: radio haloes and magnetic fields. , keywords =. doi:10.1093/mnras/sty2206 , archivePrefix =. 1707.03396 , primaryClass =

    Pith/arXiv arXiv

  18. [18]

    , keywords =

    Simulating galaxy formation with the IllustrisTNG model. , keywords =. doi:10.1093/mnras/stx2656 , archivePrefix =. 1703.02970 , primaryClass =

    Pith/arXiv arXiv

  19. [19]

    , keywords =

    First results from the IllustrisTNG simulations: matter and galaxy clustering. , keywords =. doi:10.1093/mnras/stx3304 , archivePrefix =. 1707.03397 , primaryClass =

    Pith/arXiv arXiv

  20. [20]

    Computational Astrophysics and Cosmology , keywords =

    The IllustrisTNG simulations: public data release. Computational Astrophysics and Cosmology , keywords =. doi:10.1186/s40668-019-0028-x , archivePrefix =. 1812.05609 , primaryClass =

    Pith/arXiv arXiv

  21. [21]

    Synthesis of environmental and star-forming regulation mechanisms

    Semi-analytic galaxies - I. Synthesis of environmental and star-forming regulation mechanisms. , keywords =. doi:10.1093/mnras/sty1131 , archivePrefix =. 1801.03883 , primaryClass =

    Pith/arXiv arXiv

  22. [22]

    , 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

  23. [23]

    , keywords =

    MULTIDARK-GALAXIES: data release and first results. , keywords =. doi:10.1093/mnras/stx2662 , archivePrefix =. 1710.08150 , primaryClass =

    Pith/arXiv arXiv

  24. [24]

    Boletin de la Asociacion Argentina de Astronomia La Plata Argentina , keywords =

    Models of galaxy formation and evolution. Boletin de la Asociacion Argentina de Astronomia La Plata Argentina , keywords =

  25. [26]

    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

  26. [27]

    , keywords =

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

    Pith/arXiv arXiv

  27. [28]

    , keywords =

    On the environmental influence of groups and clusters of galaxies beyond the virial radius: Galactic conformity at few Mpc scales. , keywords =. doi:10.1093/mnras/stac1020 , archivePrefix =. 2110.09536 , primaryClass =

    Pith/arXiv arXiv

  28. [29]

    , keywords =

    Ayromlou,. , keywords =

  29. [30]

    Monthly Notices of the Royal Astronomical Society , volume =

    Wang, Kai and Peng, Yingjie and Chen, Yangyao , title = ". Monthly Notices of the Royal Astronomical Society , volume =. 2023 , month =. doi:10.1093/mnras/stad1169 , url =

    work page doi:10.1093/mnras/stad1169 2023

  30. [31]

    The Environmental Quenching Mechanisms of Field Dwarf Galaxies , journal =

    Benavides, Jos. The Environmental Quenching Mechanisms of Field Dwarf Galaxies , journal =. 2025 , month =. doi:10.3847/1538-4357/adced0 , url =

    work page doi:10.3847/1538-4357/adced0 2025

  31. [32]

    , keywords =

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

    Pith/arXiv arXiv

  32. [33]

    , keywords =

    The Eighth Data Release of the Sloan Digital Sky Survey: First Data from SDSS-III. , keywords =. doi:10.1088/0067-0049/193/2/29 , archivePrefix =. 1101.1559 , primaryClass =

    Pith/arXiv arXiv

  33. [34]

    , title =

    Adhikari, Susmita and Dalal, Neal and Chamberlain, Robert T. , title =. 2014 , month =. doi:10.1088/1475-7516/2014/11/019 , url =

    doi:10.1088/1475-7516/2014/11/019 2014

  34. [35]

    , title =

    More, Surhud and Diemer, Benedikt and Kravtsov, Andrey V. , title =. 2015 , month =. doi:10.1088/0004-637X/810/1/36 , url =

    doi:10.1088/0004-637x/810/1/36 2015

  35. [36]

    , keywords =

    Universal at Last? The Splashback Mass Function of Dark Matter Halos. , keywords =. doi:10.3847/1538-4357/abbf52 , archivePrefix =. 2007.10346 , primaryClass =

    Pith/arXiv arXiv 2007

  36. [37]

    , keywords =

    Galaxy Cluster Mass Estimation through the Splashback Radius. , keywords =. doi:10.3847/1538-4357/ade308 , archivePrefix =. 2506.07425 , primaryClass =

    Pith/arXiv arXiv

  37. [38]

    2024 , month =

    Xu, Weiwei and Shan, Huanyuan and Li, Ran and Yao, Ji and Wang, Chunxiang and Li, Nan and Zhang, Chaoli , title =. 2024 , month =. doi:10.3847/1538-4357/ad57c7 , url =

    doi:10.3847/1538-4357/ad57c7 2024

  38. [39]

    , keywords =

    The galaxy bias profile of cosmic voids. , keywords =. doi:10.1051/0004-6361/202555221 , archivePrefix =. 2504.14616 , primaryClass =

    arXiv

  39. [40]

    , keywords =

    The dependence of assembly bias on the cosmic web. , keywords =. doi:10.1093/mnras/stae796 , archivePrefix =. 2309.12401 , primaryClass =

    Pith/arXiv arXiv

  40. [41]

    , keywords =

    Traces of the evolution of cosmic void galaxies: An integral field spectroscopy-based analysis. , keywords =. doi:10.1051/0004-6361/202453110 , archivePrefix =. 2506.07783 , primaryClass =

    Pith/arXiv arXiv

  41. [42]

    , keywords =

    The evolutionary path of void galaxies in TNG300 simulation. , keywords =. doi:10.1093/mnras/stae193 , archivePrefix =. 2312.09297 , primaryClass =

    Pith/arXiv arXiv

  42. [43]

    Boletin de la Asociacion Argentina de Astronomia La Plata Argentina , keywords =

    Propiedades astrof \' sicas de galaxias en los entornos de vac \' os cosmol \'o gicos. Boletin de la Asociacion Argentina de Astronomia La Plata Argentina , keywords =

  43. [44]

    , 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

  44. [45]

    , keywords =

    Relative effect of nodes and filaments of the cosmic web on the quenching of galaxies and the orientation of their spin. , keywords =. doi:10.1051/0004-6361/202141723 , archivePrefix =. 2109.14623 , primaryClass =

    Pith/arXiv arXiv

  45. [46]

    Monthly Notices of the Royal Astronomical Society , volume =

    Stephenson, H M O and Stott, J P and Butler, J and Webster, M and Head, J , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2025 , month =. doi:10.1093/mnras/staf120 , url =

    doi:10.1093/mnras/staf120 2025

  46. [47]

    arXiv e-prints , keywords =

    Environmental history of filament galaxies: stellar mass assembly and star-formation of filament galaxies. arXiv e-prints , keywords =. doi:10.48550/arXiv.2509.17697 , archivePrefix =. 2509.17697 , primaryClass =

    doi:10.48550/arxiv.2509.17697

  47. [48]

    , 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

  48. [49]

    and Rudnick, Gregory and Jablonka, Pascale and Ramatsoku, Mpati and Nagaraj, Gautam and Vulcani, Benedetta and Koopmann, Rebecca A

    Finn, Rose A. and Rudnick, Gregory and Jablonka, Pascale and Ramatsoku, Mpati and Nagaraj, Gautam and Vulcani, Benedetta and Koopmann, Rebecca A. and Fossati, Matteo and Agostino, James and Bah. Virgo Filaments. V. Disrupting the Baryon Cycle in the NGC 5364 Galaxy Group , journal =. 2025 , month =. doi:10.3847/1538-4357/adc566 , url =

    doi:10.3847/1538-4357/adc566 2025

  49. [50]

    Monthly Notices of the Royal Astronomical Society , volume =

    Navdha and Busch, Philipp and White, Simon D M , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2025 , month =. doi:10.1093/mnras/staf578 , url =

    doi:10.1093/mnras/staf578 2025

  50. [51]

    , 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

  51. [52]

    , keywords =

    Characterizing HOD in filaments and nodes of the cosmic web. , keywords =. doi:10.1093/mnras/stae188 , archivePrefix =. 2310.19928 , primaryClass =

    Pith/arXiv arXiv

  52. [53]

    , year = 2026, month = jan, doi =

    The galaxy-environment connection revealed by constrained simulations. , year = 2026, month = jan, doi =

    2026

  53. [54]

    , keywords =

    Caught in the Cosmic Web: Evidence for Ram Pressure Stripping of a Low-mass Galaxy by the Cosmic Web. , keywords =. doi:10.3847/2041-8213/ae0b5e , archivePrefix =. 2509.15405 , primaryClass =

    arXiv 2041

  54. [55]

    arXiv e-prints , keywords =

    Connecting clustering and the cosmic web:Observational constraints on secondary halo bias. arXiv e-prints , keywords =. doi:10.48550/arXiv.2511.19607 , archivePrefix =. 2511.19607 , primaryClass =

    work page doi:10.48550/arxiv.2511.19607

  55. [56]

    , keywords =

    Galaxy group spin alignment with cosmic filament in the TNG simulation. , keywords =. doi:10.1088/1475-7516/2025/10/095 , archivePrefix =. 2508.20494 , primaryClass =

    arXiv 2025

  56. [57]

    Filament identification and properties

    Galaxies in the simulated cosmic web: I. Filament identification and properties. , keywords =. doi:10.1051/0004-6361/202554079 , archivePrefix =. 2502.06484 , primaryClass =

    arXiv

  57. [58]

    , 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

  58. [59]

    10.1051/0004-6361/202555329

    Assessing the connection between galactic conformity and assembly-type bias , DOI= "10.1051/0004-6361/202555329", url= "https://doi.org/10.1051/0004-6361/202555329", journal =

    doi:10.1051/0004-6361/202555329

  59. [60]

    , keywords =

    Backsplash galaxies and their impact on galaxy evolution: a three-stage, four-type perspective. , keywords =. doi:10.1093/mnras/stad2267 , archivePrefix =. 2307.13037 , primaryClass =

    Pith/arXiv arXiv

  60. [61]

    , keywords =

    Leavers and remainers: galaxies split by group-exit. , keywords =. doi:10.1093/mnras/stz2829 , archivePrefix =. 1910.03618 , primaryClass =

    Pith/arXiv arXiv 1910

  61. [62]

    , keywords =

    Why does the environmental influence on group and cluster galaxies extend beyond the virial radius?. , keywords =. doi:10.1093/mnras/stt109 , archivePrefix =. 1210.8407 , primaryClass =

    Pith/arXiv arXiv

  62. [63]

    , keywords =

    Do galaxy mergers prefer under-dense environments?. , keywords =. doi:10.1051/0004-6361/202347705 , archivePrefix =. 2402.18520 , primaryClass =

    Pith/arXiv arXiv

  63. [64]

    , keywords =

    Galaxy mergers in Subaru HSC-SSP: A deep representation learning approach for identification, and the role of environment on merger incidence. , keywords =. doi:10.1051/0004-6361/202346743 , archivePrefix =. 2309.15539 , primaryClass =

    Pith/arXiv arXiv

  64. [65]

    , keywords =

    On the occurrence of galaxy harassment. , keywords =. doi:10.1051/0004-6361/201425235 , archivePrefix =. 1503.01965 , primaryClass =

    Pith/arXiv arXiv

  65. [66]

    , keywords =

    Large-scale Structures in the CANDELS Fields: The Role of the Environment in Star Formation Activity. , keywords =. doi:10.3847/1538-4357/ab61fd , archivePrefix =. 1912.04890 , primaryClass =

    Pith/arXiv arXiv 1912

  66. [67]

    , keywords =

    Is main-sequence galaxy star formation controlled by halo mass accretion?. , keywords =. doi:10.1093/mnras/stv2513 , archivePrefix =. 1508.04842 , primaryClass =

    Pith/arXiv arXiv

  67. [68]

    , keywords =

    The Stellar-to-Halo Mass Relation of Local Galaxies Segregates by Color. , keywords =. doi:10.1088/0004-637X/799/2/130 , archivePrefix =. 1408.5407 , primaryClass =

    Pith/arXiv arXiv

  68. [69]

    , keywords =

    The Eighteenth Data Release of the Sloan Digital Sky Surveys: Targeting and First Spectra from SDSS-V. , keywords =. doi:10.3847/1538-4365/acda98 , archivePrefix =. 2301.07688 , primaryClass =

    Pith/arXiv arXiv

  69. [70]

    and Cacciato, Marcello and Skibba, Ramin and Mo, H

    More, Surhud and van den Bosch, Frank C. and Cacciato, Marcello and Skibba, Ramin and Mo, H. J. and Yang, Xiaohu , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2010 , month =. doi:10.1111/j.1365-2966.2010.17436.x , url =

    arXiv 2010

  70. [71]

    and Leauthaud, Alexie and Bundy, Kevin and George, Matthew R

    Tinker, Jeremy L. and Leauthaud, Alexie and Bundy, Kevin and George, Matthew R. and Behroozi, Peter and Massey, Richard and Rhodes, Jason and Wechsler, Risa H. , title =. 2013 , month =. doi:10.1088/0004-637X/778/2/93 , url =

    doi:10.1088/0004-637x/778/2/93 2013

  71. [72]

    Monthly Notices of the Royal Astronomical Society , volume =

    Mandelbaum, Rachel and Wang, Wenting and Zu, Ying and White, Simon and Henriques, Bruno and More, Surhud , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2016 , month =. doi:10.1093/mnras/stw188 , url =

    doi:10.1093/mnras/stw188 2016

  72. [73]

    Monthly Notices of the Royal Astronomical Society , volume =

    Lange, Johannes U and van den Bosch, Frank C and Zentner, Andrew R and Wang, Kuan and Villarreal, Antonia Sierra , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2019 , month =. doi:10.1093/mnras/stz1466 , url =

    work page doi:10.1093/mnras/stz1466 2019

  73. [74]

    Monthly Notices of the Royal Astronomical Society , volume =

    Kauffmann, Guinevere and Li, Cheng and Zhang, Wei and Weinmann, Simone , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2013 , month =. doi:10.1093/mnras/stt007 , url =

    doi:10.1093/mnras/stt007 2013

  74. [75]

    and Watson, Douglas F

    Hearin, Andrew P. and Watson, Douglas F. and Bosch, Frank C. van den , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2015 , month =. doi:10.1093/mnras/stv1358 , url =

    doi:10.1093/mnras/stv1358 2015

  75. [76]

    and Behroozi, Peter S

    Hearin, Andrew P. and Behroozi, Peter S. and van den Bosch, Frank C. , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2016 , month =. doi:10.1093/mnras/stw1462 , url =

    doi:10.1093/mnras/stw1462 2016

  76. [77]

    Monthly Notices of the Royal Astronomical Society , volume =

    Kauffmann, Guinevere , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2015 , month =. doi:10.1093/mnras/stv2113 , url =

    doi:10.1093/mnras/stv2113 2015

  77. [78]

    , keywords =

    Galactic conformity measured in semi-analytic models. , keywords =. doi:10.1093/mnras/stx3253 , archivePrefix =. 1703.10175 , primaryClass =

    Pith/arXiv arXiv

  78. [79]

    Correlating galaxy colour and halo concentration: a tunable halo model of galactic conformity , journal =

    Paranjape, Aseem and Kova. Correlating galaxy colour and halo concentration: a tunable halo model of galactic conformity , journal =. 2015 , month =. doi:10.1093/mnras/stv2137 , url =

    doi:10.1093/mnras/stv2137 2015

  79. [80]

    , keywords =

    The manifestation of secondary bias on the galaxy population from IllustrisTNG300. , keywords =. doi:10.1093/mnras/staa1624 , archivePrefix =. 2001.01739 , primaryClass =

    Pith/arXiv arXiv 2001

  80. [81]

    , keywords =

    The impact of assembly bias on the halo occupation in hydrodynamical simulations. , keywords =. doi:10.1093/mnras/sty2110 , archivePrefix =. 1805.06938 , primaryClass =

    Pith/arXiv arXiv

Showing first 80 references.