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arxiv: 2606.28151 · v1 · pith:U6OBT2GCnew · submitted 2026-06-26 · 🌌 astro-ph.CO · gr-qc

The effect of dark energy on the void-halo perpendicular alignments

Geonwoo Kang , Jounghun Lee (Seoul National University) This is my paper

Pith reviewed 2026-06-29 02:52 UTC · model grok-4.3

classification 🌌 astro-ph.CO gr-qc
keywords dark energycosmic voidsgalactic halosperpendicular alignmentscosmological simulationswCDMvoid-halo alignments
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The pith

In faster-accelerating universes galactic halos on void surfaces align more strongly perpendicular to the lines toward void centers.

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

The paper compares halo catalogs from simulations that share the same initial conditions but differ only in the dark energy equation of state. For each cosmology it locates voids at z=0.1, selects the halos on their surfaces, and measures the distribution p(cos theta) of the angle between each halo's shape axis and the direction to the void center. After removing spurious trends caused by differing halo mass and sphericity distributions, a single fitted parameter d_t quantifies how perpendicular the alignments are. d_t rises systematically when dark energy pressure is more negative and evolves more rapidly, leading the authors to propose a bilinear model that relates d_t to the dark energy parameters w and wa.

Core claim

In cosmologies where dark energy has more negative pressure and evolves more rapidly, the perpendicular alignments of void-surface galactic halos become stronger, as measured by higher values of the single parameter d_t in the empirically modified linear-theory formula for p(cos theta).

What carries the argument

The single parameter d_t that sets the amplitude of the perpendicular-alignment term in the analytic fit to p(cos theta).

If this is right

  • d_t takes higher values in models where dark energy pressure is more negative or changes faster.
  • A bilinear relation between the two cases w equals -1 and w not equal to -1 describes the numerical d_t differences to high accuracy.
  • The strength of void-surface halo perpendicular alignments can serve as an independent indicator of whether dark energy is dynamic.

Where Pith is reading between the lines

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

  • If the d_t signal is recovered in observational data it would supply a new route to constrain the time evolution of dark energy that does not rely on distance-redshift measurements.
  • The same alignment statistic could be measured at higher redshift in future surveys to track how the dark-energy effect grows with time.

Load-bearing premise

The empirically modified single-parameter analytic formula derived from linear perturbation theory accurately captures the shape of p(cos theta) across all cosmologies without introducing additional cosmology-dependent biases.

What would settle it

Extract d_t from observed galaxy shapes and void catalogs in a real survey and test whether its values follow the same bilinear dependence on w and wa that appears in the simulations.

read the original abstract

We report a numerical discovery that in a more rapidly accelerating spacetime, the galactic halos on void surfaces develop stronger perpendicular alignments with the directions toward the void centers. We utilize the halo catalogs from the AbacusSummit suite of simulations for $10$ different cosmologies that include one Planck $\Lambda$CDM, four $w$CDM and five $w_{0}w_{a}$CDM, which share the identical initial conditions except for the dark energy equation of state. For each cosmology, we identify the voids and void-surface galactic halos at $z=0.1$ and determine the probability density functions of the cosines of the angles, $p(\cos\theta)$, between the shape axes of void-surface galactic halos and the directions toward the void centers. The numerically obtained $p(\cos\theta)$ is fitted to an analytic single-parameter formula derived through an empirical modification of the linear perturbation theory. Eliminating spurious signals caused by the differences in the mass and sphericity distributions of void-surface galactic halos among different cosmologies, we detect a clear net effect of dark energy on the strengths of the perpendicular alignments of void-surface galactic halos, quantified by the single parameter, $d_{t}$. Noting that $d_{t}$ has higher values in the cosmologies where dark energy has more negative pressure and evolves more rapidly, we put forth a bilinear model for the difference in $d_{t}$ between the two cases of $w=-1$ and $w\ne -1$. Demonstrating that this bilinear relation excellently describes the numerical results, we conclude that the perpendicular alignments of void-surface galactic halos should in principle be a powerful independent indicator of the dynamic nature of dark energy.

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 / 2 minor

Summary. The manuscript reports a numerical study using AbacusSummit simulations across 10 cosmologies (one Planck ΛCDM, four wCDM, five w0waCDM) with identical initial conditions. Voids and void-surface galactic halos are identified at z=0.1; the probability density p(cos θ) between halo shape axes and void-center directions is measured and fitted to a single-parameter analytic formula obtained via empirical modification of linear perturbation theory. After re-weighting to remove mass and sphericity selection biases, the fit parameter d_t is shown to increase for cosmologies with more negative and rapidly evolving dark-energy pressure. A bilinear model relating Δd_t to the deviation from w=-1 is fitted to these d_t values and reported to describe the results well, leading to the claim that void-halo perpendicular alignments can serve as an independent probe of dynamic dark energy.

Significance. If the central result holds, the work would introduce a new large-scale-structure observable sensitive to the dynamical nature of dark energy, complementing standard probes. The use of shared initial conditions across cosmologies is a clear methodological strength that isolates dark-energy effects. The explicit correction for mass and sphericity distributions is also a positive step. However, the two-stage fitting procedure (first extracting d_t from an empirical template, then fitting a bilinear model to those d_t values) and the lack of independent cross-validation limit the immediate impact.

major comments (3)
  1. [Abstract and fitting section] Abstract and the section describing the analytic fit: the single-parameter formula is an empirical modification of linear perturbation theory rather than a first-principles derivation. The manuscript must demonstrate that fit residuals are uncorrelated with w and w_a; otherwise any cosmology-dependent mismatch in the template (e.g., in the wings or near cos θ = 0) is absorbed into d_t and can produce or mask the reported bilinear trend.
  2. [Results on bilinear model] Results section on the bilinear model: d_t is defined as the fit parameter to the observed p(cos θ) for each cosmology, after which the bilinear relation is fitted directly to the resulting d_t values. This two-step construction requires an independent cross-check (different statistic, different void finder, or external simulation suite) to establish that the claimed dark-energy dependence is not an artifact of the chosen functional form.
  3. [Bias-correction section] Section on mass/sphericity re-weighting: while the leading-order selection biases are addressed, the paper should quantify whether residual higher-order biases or their interaction with the PT-motivated template remain cosmology-dependent and affect the extracted d_t trend.
minor comments (2)
  1. [Abstract] Clarify in the abstract and methods whether the single Planck ΛCDM run is counted separately from the four wCDM runs or is one of them.
  2. [Abstract] Notation: the symbol d_t is introduced without an explicit equation reference in the abstract; add a parenthetical reference to the defining equation when first mentioned.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the constructive review and for highlighting the strengths of our shared-initial-conditions approach. We address each major comment below with specific plans for revision.

read point-by-point responses

  1. Referee: [Abstract and fitting section] Abstract and the section describing the analytic fit: the single-parameter formula is an empirical modification of linear perturbation theory rather than a first-principles derivation. The manuscript must demonstrate that fit residuals are uncorrelated with w and w_a; otherwise any cosmology-dependent mismatch in the template (e.g., in the wings or near cos θ = 0) is absorbed into d_t and can produce or mask the reported bilinear trend.

    Authors: We agree that explicit verification of fit quality across cosmologies is necessary. In the revised manuscript we will add a dedicated subsection presenting the residuals of the single-parameter template for all ten cosmologies. These residuals will be shown to be small (typically < 5 % of the peak height) and to exhibit no systematic correlation with w or w_a, thereby confirming that the reported trend in d_t is not driven by template mismatch. revision: yes

  2. Referee: [Results on bilinear model] Results section on the bilinear model: d_t is defined as the fit parameter to the observed p(cos θ) for each cosmology, after which the bilinear relation is fitted directly to the resulting d_t values. This two-step construction requires an independent cross-check (different statistic, different void finder, or external simulation suite) to establish that the claimed dark-energy dependence is not an artifact of the chosen functional form.

    Authors: We acknowledge the two-stage nature of the analysis. The shared initial conditions already isolate dark-energy effects from cosmic variance, which is a key strength. In revision we will test robustness by repeating the d_t extraction with a second, qualitatively different functional form and demonstrating that the bilinear trend persists. A full external cross-validation with an independent simulation suite lies beyond the scope of the present work and will be noted as future work; we therefore regard the requested cross-check as only partially addressable at this stage. revision: partial

  3. Referee: [Bias-correction section] Section on mass/sphericity re-weighting: while the leading-order selection biases are addressed, the paper should quantify whether residual higher-order biases or their interaction with the PT-motivated template remain cosmology-dependent and affect the extracted d_t trend.

    Authors: We will expand the bias-correction section to include a quantitative assessment of residual higher-order biases. Specifically, we will compute the post-reweighting residuals in mass and sphericity moments and test for any remaining cosmology dependence. We will also compare d_t values obtained with and without the re-weighting step to isolate any interaction between the bias correction and the template, thereby confirming that the dark-energy trend is robust. revision: yes

Circularity Check

0 steps flagged

No significant circularity detected

full rationale

The paper extracts d_t by fitting an empirically modified linear PT formula to measured p(cos θ) distributions from independent simulations for each cosmology, applies mass/sphericity reweighting to remove selection effects, and then fits a bilinear model to the resulting d_t values to describe their variation with w and w_a. This sequence is standard empirical analysis rather than a derivation that reduces to its inputs by construction. No quoted step equates a claimed prediction or first-principles result to a fitted parameter or self-citation chain; the central claim of a net DE dependence rests on the variation across cosmologies after corrections and is self-contained against the simulation data.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The claim depends on an empirically modified linear perturbation theory formula whose validity across cosmologies is assumed, plus the isolation of the dark energy effect after bias correction; d_t and the bilinear coefficients are fitted quantities.

free parameters (2)
  • d_t
    Single fit parameter quantifying perpendicular alignment strength in the analytic formula for each cosmology.
  • bilinear model coefficients
    Parameters of the bilinear relation fitted to the set of d_t values across the ten cosmologies.
axioms (1)
  • standard math Linear perturbation theory supplies the base form for the halo alignment distribution p(cos theta)
    The analytic formula is described as an empirical modification of linear perturbation theory.

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discussion (0)

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Reference graph

Works this paper leans on

30 extracted references · 28 canonical work pages · 17 internal anchors

  1. [1]

    Voids in the PSCz Survey and the Updated Zwicky Catalog

    F. Hoyle and M. S. Vogeley,Voids in the pscz survey and the updated zwicky catalog, Astrophys. J.566(2002) 641, doi:10.1086/338340 [arXiv:astro-ph/0109357 [astro-ph]]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/338340 2002

  2. [2]

    Kang and J

    G. Kang and J. Lee,How the cosmic voids contribute to stalling and quenching the giant galaxies on their surfaces, JCAP04(2026), 013 doi:10.1088/1475-7516/2026/04/013 [arXiv:2508.12283 [astro-ph.CO]]

    work page doi:10.1088/1475-7516/2026/04/013 2026

  3. [3]

    2018, Monthly Notices of the Royal Astronomical Society, 480, 5113, doi:10.1093/mnras/sty2206

    F. Marinacci, M. Vogelsberger, R. Pakmor, P. Torrey, V. Springel, L. Hernquist, D. Nelson, R. Weinberger, A. Pillepich and J. Naiman,et al. First results from the IllustrisTNG simulations: radio haloes and magnetic fields, Mon. Not. Roy. Astron. Soc.480(2018) 5113, doi:10.1093/mnras/sty2206 [arXiv:1707.03396 ]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2206 2018

  4. [4]

    J. P. Naimanet al. First results from the IllustrisTNG simulations: a tale of two elements - chemical evolution of magnesium and europium, Mon. Not. Roy. Astron. Soc.477(2018) 1206, doi:10.1093/mnras/sty618 [arXiv:1707.03401 [astro-ph.GA]]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty618 2018

  5. [5]

    2018, MNRAS, 475, 624, doi: 10.1093/mnras/stx3040

    D. Nelson, A. Pillepich, V. Springel, R. Weinberger, L. Hernquist, R. Pakmor, S. Genel, P. Torrey, M. Vogelsberger and G. Kauffmann,et al. First results from the IllustrisTNG simulations: the galaxy colour bimodality, Mon. Not. Roy. Astron. Soc.475(2018) 624, doi:10.1093/mnras/stx3040 [arXiv:1707.03395 [astro-ph.GA]]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx3040 2018

  6. [6]

    2018, MNRAS, 475, 648, doi:10.1093/mnras/stx3112 Planck Collaboration, Ade, P

    A. Pillepich, D. Nelson, L. Hernquist, V. Springel, R. Pakmor, P. Torrey, R. Weinberger, S. Genel, J. Naiman and F. Marinacci,et al. First results from the IllustrisTNG simulations: the stellar mass content of groups and clusters of galaxies, Mon. Not. Roy. Astron. Soc.475 (2018) 648, doi:10.1093/mnras/stx3112 [arXiv:1707.03406 ]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx3112 2018

  7. [7]

    First results from the IllustrisTNG simulations: matter and galaxy clustering

    V. Springel, R. Pakmor, A. Pillepich, R. Weinberger, D. Nelson, L. Hernquist, M. Vogelsberger, S. Genel, P. Torrey and F. Marinacci,et al. First results from the IllustrisTNG simulations: matter and galaxy clustering, Mon. Not. Roy. Astron. Soc.475(2018) 676, doi:10.1093/mnras/stx3304 [arXiv:1707.03397 ]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx3304 2018

  8. [8]

    2019, Computational Astrophysics and Cosmology, 6, 2, doi: 10.1186/s40668-019-0028-x

    D. Nelson, V. Springel, A. Pillepich, V. Rodriguez-Gomez, P. Torrey, S. Genel, M. Vogelsberger, R. Pakmor, F. Marinacci and R. Weinberger,et al. The IllustrisTNG Simulations: Public Data Release, Comput. Astrophys. Cosmol.6(2019) 2, doi:10.1186/s40668-019-0028-x [arXiv:1812.05609 [astro-ph.GA]]

    work page doi:10.1186/s40668-019-0028-x 2019

  9. [9]

    K. J. Ludwick,The viability of phantom dark energy: A review, Mod. Phys. Lett. A32(2017) no.28, 1730025 doi:10.1142/S0217732317300257 [arXiv:1708.06981 [astro-ph.CO]]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1142/s0217732317300257 2017

  10. [10]

    Cosmological Consequences of a Rolling Homogeneous Scalar Field

    B. Ratra and P. J. E. Peebles,Cosmological Consequences of a Rolling Homogeneous Scalar Field, Phys. Rev. D37(1988) 3406, doi:10.1103/PhysRevD.37.3406

    work page doi:10.1103/physrevd.37.3406 1988

  11. [11]

    Cosmology and the Fate of Dilatation Symmetry

    C. Wetterich,Cosmology and the Fate of Dilatation Symmetry, Nucl. Phys. B302(1988), 668-696 doi:10.1016/0550-3213(88)90193-9 [arXiv:1711.03844 [hep-th]]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/0550-3213(88)90193-9 1988

  12. [12]

    Accelerating Universes with Scaling Dark Matter

    M. Chevallier and D. Polarski,Accelerating universes with scaling dark matter, Int. J. Mod. Phys. D10(2001), 213-224 doi:10.1142/S0218271801000822 [arXiv:gr-qc/0009008 [gr-qc]]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1142/s0218271801000822 2001

  13. [13]

    E. V. Linder,Exploring the expansion history of the universe, Phys. Rev. Lett.90(2003), 091301 doi:10.1103/PhysRevLett.90.091301 [arXiv:astro-ph/0208512 [astro-ph]]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.90.091301 2003

  14. [14]

    Revisiting the Galaxy Shape and Spin Alignments with the Large-Scale Tidal Field: An Effective Practical Model

    J. Lee,Revisiting the Galaxy Shape and Spin Alignments with the Large-Scale Tidal Field: An Effective Practical Model, Astrophys. J.872(2019) no.1, 37 doi:10.3847/1538-4357/aafe11 [arXiv:1808.08559 [astro-ph.CO]]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aafe11 2019

  15. [15]

    N. A. Maksimova, L. H. Garrison, D. J. Eisenstein, et al.,AbacusSummit: a massive set of high-accuracy, high-resolution N-body simulations, Mon. Not. Roy. Astron. Soc.508(2021) 4037, doi:10.1093/mnras/stab2484 [arXiv:2110.11398 [astro-ph.CO]]. – 16 –

    work page doi:10.1093/mnras/stab2484 2021

  16. [17]

    L. H. Garrison, D. J. Eisenstein, D. Ferrer, N. A. Maksimova and P. A. Pinto,The abacus cosmological N-body code, Mon. Not. Roy. Astron. Soc.508(2021) 575, doi:10.1093/mnras/stab2482 [arXiv:2110.11392 [astro-ph.CO]]

    work page doi:10.1093/mnras/stab2482 2021

  17. [18]

    The Cosmic Linear Anisotropy Solving System (CLASS) I: Overview

    J. Lesgourgues,The Cosmic Linear Anisotropy Solving System (CLASS) I: Overview(2011) arXiv e-prints. doi:10.48550/arXiv.1104.2932

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1104.2932 2011

  18. [19]

    M. V. L. Metchnik,A fast N-body scheme for computational cosmology, Ph.D. Thesis. U. of Arizona (2009)

    2009

  19. [21]

    Hadzhiyska, D

    B. Hadzhiyska, D. J. Eisenstein, S. Bose, et al.,Halo occupation distribution modeling in AbacusSummit simulations, Mon. Not. Roy. Astron. Soc.509(2022) 501, doi:10.1093/mnras/stab2980 [arXiv:2110.11399 [astro-ph.CO]]

    work page doi:10.1093/mnras/stab2980 2022

  20. [22]

    M. S. Warren, P. J. Quinn, J. K. Salmon, W. H. Zurek,Dark Halos Formed via Dissipationless Collapse. I. Shapes and Alignment of Angular Momentum., Astrophys. J.399(1992) 405, doi:10.1086/171937

    work page doi:10.1086/171937 1992

  21. [23]

    Planck 2018 results. VI. Cosmological parameters

    N. Aghanimet al.[Planck],Planck 2018 results. VI. Cosmological parameters, Astron. Astrophys.641(2020) A6, doi:10.1051/0004-6361/201833910 [arXiv:1807.06209 [astro-ph.CO]]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833910 2018

  22. [24]

    Kang and J

    G. Kang and J. Lee,Void spin distribution as a powerful probe ofσ8, JCAP06(2025), 011 doi:10.1088/1475-7516/2025/06/011 [arXiv:2501.09476 [astro-ph.CO]]

    work page doi:10.1088/1475-7516/2025/06/011 2025

  23. [25]

    P. Bett, V. Eke, C. S. Frenk, A. Jenkins, J. Helly and J. Navarro,The spin and shape of dark matter haloes in the Millennium simulation of a lambda-CDM universe, Mon. Not. Roy. Astron. Soc.376(2007) 215, doi:10.1111/j.1365-2966.2007.11432.x [arXiv:astro-ph/0608607 [astro-ph]]

    work page doi:10.1111/j.1365-2966.2007.11432.x 2007

  24. [26]

    A. G. Adameet al.[DESI],DESI 2024 VI: cosmological constraints from the measurements of baryon acoustic oscillations, JCAP02(2025) 021, doi:10.1088/1475-7516/2025/02/021 [arXiv:2404.03002 ]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1475-7516/2025/02/021 2024

  25. [27]

    D. A. Dicus and W. W. Repko,Constraints on the dark energy equation of state from recent supernova data, Phys. Rev. D70(2004), 083527 doi:10.1103/PhysRevD.70.083527 [arXiv:astro-ph/0407094 [astro-ph]]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.70.083527 2004

  26. [28]

    D. O. Jones, K. S. Mandel, R. P. Kirshner, S. Thorp, P. M. Challis, A. Avelino, D. Brout, C. Burns, R. J. Foley and Y. C. Pan,et al. Cosmological Results from the RAISIN Survey: Using Type Ia Supernovae in the Near Infrared as a Novel Path to Measure the Dark Energy Equation of State, Astrophys. J.933(2022) no.2, 172 doi:10.3847/1538-4357/ac755b [arXiv:22...

    work page doi:10.3847/1538-4357/ac755b 2022

  27. [29]

    How Sensitive Are Weak Lensing Statistics to Dark Energy Content?

    D. Munshi and Y. Wang,How sensitive are weak lensing statistics to dark energy content?, Astrophys. J.583(2003) 566, doi:10.1086/345425 [arXiv:astro-ph/0206483 [astro-ph]]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/345425 2003

  28. [30]

    A test of the nature of cosmic acceleration using galaxy redshift distortions

    L. Guzzo, M. Pierleoni, B. Meneux, E. Branchini, O. L. Fevre, C. Marinoni, B. Garilli, J. Blaizot, G. De Lucia and A. Pollo,et al. A test of the nature of cosmic acceleration using galaxy redshift distortions, Nature451(2008) 541, doi:10.1038/nature06555 [arXiv:0802.1944 [astro-ph]]

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature06555 2008

  29. [31]

    Boyle, C

    A. Boyle, C. Uhlemann, O. Friedrich, A. Barthelemy, S. Codis, F. Bernardeau, C. Giocoli and M. Baldi,Nuw CDM cosmology from the weak-lensing convergence PDF, Mon. Not. Roy. Astron. Soc.505(2021) 2886, doi:10.1093/mnras/stab1381 [arXiv:2012.07771 [astro-ph.CO]]. – 17 –

    work page doi:10.1093/mnras/stab1381 2021

  30. [32]

    Zhang and S

    P. Zhang and S. Li,The large scale structure probes of dark energy, [arXiv:2606.24288 [astro-ph.CO]]. – 18 –

    Pith/arXiv arXiv