arxiv: 2604.26072 · v1 · submitted 2026-04-28 · 🌌 astro-ph.CO · astro-ph.GA

Recognition: unknown

Caught in the Cosmic Web: Environmental Impacts on the Halo Substructure Boosts to Dark Matter Annihilation Signals

Feven Markos Hunde, Maciej Bilicki, Wojciech A. Hellwing

Authors on Pith no claims yet

Pith reviewed 2026-05-07 14:35 UTC · model grok-4.3

classification 🌌 astro-ph.CO astro-ph.GA

keywords dark matter annihilationcosmic webhalo substructureboost factorenvironment dependencefilamentsvoidssemi-analytic models

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The pith

Dark matter annihilation boost factors from subhaloes vary with cosmic web environment at fixed halo mass.

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

The paper establishes that standard models treating the subhalo boost as a universal function of host mass miss systematic environmental effects from the cosmic web. It incorporates simulation-calibrated ratios for concentrations, subhalo abundances, and Vmax-Rmax relations into semi-analytic frameworks to compute environment-specific boosts relative to the cosmic mean. In the fiducial model this produces mass-dependent transitions for filaments, intermediate values for walls, and persistent suppression for voids. A sympathetic reader cares because indirect detection searches for dark matter signals assume uniform boosts, so environment could alter expected intensities from different regions of the universe.

Core claim

In the fiducial distance-dependent model, filament haloes show a mass-dependent transition from a ∼15% suppression at the low-mass end to a modest enhancement of ∼12% for massive hosts, wall haloes remain intermediate, while void haloes stay suppressed by roughly 30–33% across the explored host-mass range. These are deterministic predictions obtained by propagating environment-dependent ingredient ratios through two standard semi-analytic boost frameworks.

What carries the argument

The relative boost factor B(M, env)/B_CM(M), computed by propagating simulation-calibrated environment-dependent ratios for host concentrations, subhalo mass function, and Vmax–Rmax proxies through standard semi-analytic annihilation boost calculations.

Load-bearing premise

That simulation-calibrated environment-dependent ratios for host-halo concentrations, subhalo mass function, and Vmax–Rmax internal-structure proxies can be directly propagated through standard semi-analytic boost frameworks without introducing unaccounted biases or missing environmental interactions.

What would settle it

Direct comparison of the predicted relative boosts to outputs from high-resolution N-body simulations that tag haloes by environment at fixed mass and measure annihilation luminosity ratios, checking for the reported 15-to-12 percent filament transition and 30 percent void suppression.

Figures

Figures reproduced from arXiv: 2604.26072 by Feven Markos Hunde, Maciej Bilicki, Wojciech A. Hellwing.

**Figure 1.** Figure 1: FIG. 1 view at source ↗

**Figure 2.** Figure 2: FIG. 2. Total halo luminosity as a function of host halo mass view at source ↗

**Figure 3.** Figure 3: FIG. 3 view at source ↗

**Figure 4.** Figure 4: FIG. 4. Environment-dependent subhalo boost factor as a view at source ↗

**Figure 5.** Figure 5: FIG. 5. Median subhalo concentration view at source ↗

read the original abstract

The annihilation of dark matter (DM) particles is expected to produce Standard Model particles, providing a potential indirect signature of DM. The clumpy substructure of DM haloes amplifies the expected annihilation signal, an effect commonly quantified by the subhalo boost factor. Standard semi-analytic models usually treat this boost as a universal function of host-halo mass, neglecting systematic variations induced by the large-scale environment. In this work, we extend this framework by incorporating the influence of the cosmic web on subhalo populations. Using simulation-calibrated, environment-dependent ratios for host-halo concentrations, the subhalo mass function, and internal-structure proxies of subhalos based on the $V_{\max}$--$R_{\max}$ relation, we compute environment-conditioned boost predictions for haloes residing in filaments, walls, and voids. Our main result is the boost factor at fixed host-halo mass, expressed relative to the cosmic-mean prediction, $B(M,\mathrm{env})/B_{\mathrm{CM}}(M)$. We find a clear environmental modulation: in the fiducial distance-dependent model, filament haloes show a mass-dependent transition from a $\sim 15\%$ suppression at the low-mass end to a modest enhancement of $\sim 12\%$ for massive hosts, wall haloes remain intermediate, while void haloes stay suppressed by roughly $30$--$33\%$ across the explored host-mass range. These results should be interpreted as deterministic model predictions obtained by propagating environment-dependent ingredient ratios through two standard semi-analytic boost frameworks. We provide an environment-aware prescription for subhalo boosts, together with modular environmental corrections that may also be useful in indirect-detection forecasts, strong-lensing mass modeling, and related halo-population applications.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Desk Editor's Note private letter to a colleague

This paper adds environment dependence to subhalo boost factors via simulation ratios, but the quoted 10-30% modulations rest on treating concentration, subhalo mass function, and internal structure as independent.

read the letter

The main point is that at fixed host mass the subhalo boost to dark matter annihilation can shift by roughly 15% suppression to 12% enhancement in filaments, stay intermediate in walls, and drop 30-33% in voids once environment is folded in. The authors do this by taking three separate simulation-calibrated ratios and feeding them into two standard semi-analytic boost integrators, then reporting the ratio to the cosmic-mean case. That produces a clean, modular prescription that can be dropped into existing indirect-detection forecasts or halo-modeling codes without rewriting the whole framework. The work is transparent about being a propagation exercise rather than new data or a first-principles derivation, which keeps expectations realistic. The numbers are presented for a useful mass range and the distance-dependent model is highlighted as fiducial, so a reader can see where the effect is largest. The soft spot is exactly the one the stress test flags: multiplying marginal ratios assumes the three ingredients are uncorrelated once conditioned on environment. In practice the same halos set all three quantities, so covariances between concentration, subhalo abundance, and Vmax-Rmax could easily move the net boost by an amount comparable to the reported shifts. The abstract gives no joint-distribution check or covariance term, so that uncertainty is not quantified. This is the sort of paper that matters for people already running DM annihilation forecasts or strong-lensing mass models who want to add a modest environmental correction. It is not revolutionary on its own, but the implementation is straightforward enough that the community can test the covariance issue quickly. I would send it to peer review; the central calculation is reproducible from the described inputs and the limitation is clear enough that referees can focus on whether the independence assumption holds or needs a joint model.

Referee Report

1 major / 2 minor

Summary. The paper extends standard semi-analytic models of the subhalo boost factor for dark matter annihilation by incorporating cosmic-web environment dependence. It propagates simulation-calibrated, environment-specific ratios for host-halo concentration, subhalo mass function, and Vmax–Rmax internal-structure proxies through two established boost integrators to obtain the ratio B(M, env)/B_CM(M). The central claim is a mass-dependent modulation: in the fiducial distance-dependent model, filament haloes transition from ~15% suppression at low mass to ~12% enhancement at high mass, wall haloes are intermediate, and void haloes remain suppressed by 30–33% across the host-mass range explored. The results are presented as deterministic predictions from this propagation, together with modular environmental correction prescriptions.

Significance. If the propagation procedure is shown to be robust, the work supplies a concrete, environment-aware correction to boost factors that could be directly adopted in indirect-detection forecasts, strong-lensing analyses, and halo-population modeling. The modular form of the corrections and the explicit framing as model predictions (rather than fitted results) are strengths that enhance usability and reproducibility.

major comments (1)

[Propagation procedure and fiducial distance-dependent model results] The quantitative headline results (filament transition from ~15% suppression to ~12% enhancement; void suppression of 30–33%) are obtained by multiplying separate environment-dependent ratios for c(M,env), dN/dM_sub(env), and the Vmax–Rmax proxy before insertion into the boost integrators. Because these three quantities are measured from the same simulated haloes, their joint distribution within each environment may contain covariances that are not captured by the product of marginal ratios. No joint-distribution validation or covariance term is described, so the reported modulations could be biased at a level comparable to the effect sizes themselves. This assumption is load-bearing for the central claims.

minor comments (2)

[Abstract] The abstract states that the results are 'deterministic model predictions obtained by propagating environment-dependent ingredient ratios,' which is appropriately cautious; however, the explored host-mass range should be stated explicitly in the abstract for immediate context.
[Notation throughout] Notation for the cosmic-mean boost (B_CM(M)) is introduced clearly, but ensure that 'cosmic mean' versus 'CM' is used consistently in all figure labels and equations.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful reading and constructive feedback. We address the major comment on the propagation procedure below.

read point-by-point responses

Referee: The quantitative headline results (filament transition from ~15% suppression to ~12% enhancement; void suppression of 30–33%) are obtained by multiplying separate environment-dependent ratios for c(M,env), dN/dM_sub(env), and the Vmax–Rmax proxy before insertion into the boost integrators. Because these three quantities are measured from the same simulated haloes, their joint distribution within each environment may contain covariances that are not captured by the product of marginal ratios. No joint-distribution validation or covariance term is described, so the reported modulations could be biased at a level comparable to the effect sizes themselves. This assumption is load-bearing for the central claims.

Authors: We appreciate the referee highlighting the potential impact of covariances among the environment-dependent ratios. Our framework deliberately propagates the marginal ratios for concentration, subhalo mass function, and Vmax–Rmax proxy separately before insertion into the boost integrators. This choice preserves modularity, transparency, and usability, allowing independent environmental corrections to be applied or extended by other users, consistent with the referee's note on the strengths of the modular form. The manuscript explicitly presents the results as deterministic model predictions obtained by this propagation rather than as direct measurements from joint distributions. While full covariances could in principle refine the precision, the simulation calibrations show that the primary environmental trends are captured at the marginal level, and the multiplicative structure aligns with the separable nature of the boost integrators. In the revised manuscript we will add a dedicated discussion of this assumption, including a qualitative assessment of its robustness based on the simulation statistics, and insert an explicit caveat in the results section. revision: partial

Circularity Check

0 steps flagged

No circularity: external simulation ratios propagated through standard frameworks

full rationale

The paper's central procedure is to take environment-dependent ratios for concentrations, subhalo mass functions, and Vmax-Rmax proxies that are calibrated from external simulations, then insert them into two pre-existing semi-analytic boost integrators to obtain B(M,env)/B_CM(M). This is explicitly described as 'deterministic model predictions obtained by propagating environment-dependent ingredient ratios' rather than any derivation or fit performed inside the present work. No equation reduces a claimed prediction to a quantity defined or fitted by the paper itself; the inputs remain independent of the output boost ratios. No self-citation is load-bearing for the quantitative claims, and the derivation chain is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The model depends on simulation-calibrated ratios for three halo properties as external inputs; no new free parameters are introduced in the boost calculation itself.

axioms (1)

domain assumption Standard semi-analytic boost frameworks remain accurate when supplied with environment-dependent ratios for concentration, subhalo mass function, and Vmax-Rmax proxies.
The paper applies these ratios directly to two existing frameworks without additional cross-checks described in the abstract.

pith-pipeline@v0.9.0 · 5635 in / 1420 out tokens · 128243 ms · 2026-05-07T14:35:20.845206+00:00 · methodology

discussion (0)

Reference graph

Works this paper leans on

86 extracted references · 67 canonical work pages · 1 internal anchor

[1]

annihilation lumi- nosity

and employ thenexus+framework, implemented within ourCaCTusalgorithm introduced in Paper I. The CaCTuspackage provides an optimized implementation of the multi-scalenexus+algorithm [60], enabling efficient segmentation of the cosmic web across a wide dynamic range. The code, along with detailed documentation, will be made publicly available in Naidoo et a...

2020
[2]

A History of Dark Matter

G. Bertone and D. Hooper, Reviews of Modern Physics 90, 045002 (2018), arXiv:1605.04909 [astro-ph.CO]

work page Pith review arXiv 2018
[3]

Planck 2018 results. VI. Cosmological parameters

Planck Collaboration, N. Aghanim, Y. Akrami, M. Ash- down, J. Aumont, C. Baccigalupi, M. Ballardini, A. J. Banday, R. B. Barreiro, N. Bartolo, S. Basak, R. Battye, K. Benabed, J.-P. Bernard, M. Bersanelli, P. Bielewicz, J. J. Bock, J. R. Bond, J. Borrill, F. R. Bouchet, F. Boulanger, M. Bucher, C. Burigana, R. C. Butler, E. Calabrese, J.-F. Cardoso, J. Ca...

work page internal anchor Pith review arXiv 2020
[4]

Carr and F

B. Carr and F. Kuhnel, arXiv e-prints , arXiv:2110.02821 (2021), arXiv:2110.02821 [astro-ph.CO]

work page arXiv 2021
[5]

Jungman, M

G. Jungman, M. Kamionkowski, and K. Griest, Phys. Rep.267, 195 (1996), arXiv:hep-ph/9506380 [hep- ph]

work page arXiv 1996
[6]

Particle Dark Matter: Evidence, Candidates and Constraints

G. Bertone, D. Hooper, and J. Silk, Phys. Rep.405, 279 (2005), arXiv:hep-ph/0404175 [hep-ph]

work page Pith review arXiv 2005
[7]

Bringmann and C

T. Bringmann and C. Weniger, Physics of the Dark Uni- verse1, 194 (2012), arXiv:1208.5481 [hep-ph]

work page arXiv 2012
[8]

Roszkowski, E

L. Roszkowski, E. M. Sessolo, and S. Trojanowski, Re- ports on Progress in Physics81, 066201 (2018)

2018
[9]

S. J. Asztalos, L. J. Rosenberg, K. van Bibber, P. Sikivie, and K. Zioutas, Annual Review of Nuclear and Particle Science56, 293 (2006)

2006
[10]

D. J. E. Marsh, Phys. Rep.643, 1 (2016)

2016
[11]

J. L. Feng, ARA&A48, 495 (2010), arXiv:1003.0904 [astro-ph.CO]

work page arXiv 2010
[12]

Kopp, arXiv e-prints , arXiv:2109.00767 (2021), arXiv:2109.00767 [hep-ph]

J. Kopp, arXiv e-prints , arXiv:2109.00767 (2021), arXiv:2109.00767 [hep-ph]

work page arXiv 2021
[13]

Marrodán Undagoitia and L

T. Marrodán Undagoitia and L. Rauch, Journal of Physics G Nuclear Physics43, 013001 (2016), arXiv:1509.08767 [physics.ins-det]

work page arXiv 2016
[14]

Battaglieri, A

M. Battaglieri, A. Belloni, A. Chou, P. Cushman, B. Echenard, R. Essig, J. Estrada, J. L. Feng, B. Flaugher, P. J. Fox, P. Graham, C. Hall, R. Harnik, J. Hewett, J. Incandela, E. Izaguirre, D. McKinsey, M. Pyle, N. Roe, G. Rybka, P. Sikivie, T. M. P. Tait, N. Toro, R. Van De Water, N. Weiner, K. Zurek, E. Adelberger, A. Afanasev, D. Alexander, J. Alexande...

work page arXiv 2017
[15]

M. A. Sánchez-Conde and F. Prada, MNRAS442, 2271 (2014), arXiv:1312.1729 [astro-ph.CO]

work page arXiv 2014
[16]

Prada, MNRAS466, 4974 (2017), arXiv:1603.04057 [astro-ph.CO]

Á.Moliné, M.A.Sánchez-Conde, S.Palomares-Ruiz,and F. Prada, MNRAS466, 4974 (2017), arXiv:1603.04057 [astro-ph.CO]

work page arXiv 2017
[17]

S. Ando, T. Ishiyama, and N. Hiroshima, Galaxies7, 68 (2019), arXiv:1903.11427 [astro-ph.CO]

work page arXiv 2019
[18]

Colafrancesco, S

S. Colafrancesco, S. Profumo, and P. Ullio, A&A455, 21 (2006), arXiv:astro-ph/0507575 [astro-ph]

work page arXiv 2006
[19]

Kamionkowski, S

M. Kamionkowski, S. M. Koushiappas, and M. Kuhlen, Phys. Rev. D81, 043532 (2010), arXiv:1001.3144 [astro- ph.GA]

work page arXiv 2010
[20]

Pearson, H

J. Pearson, H. Dickinson, S. Sinha, and S. Serjeant, arXiv e-prints , arXiv:2509.22609 (2025), arXiv:2509.22609 [astro-ph.CO]

work page arXiv 2025
[21]

J. R. Bond, L. Kofman, and D. Pogosyan, Nature380, 10.1038/380603a0 (1996)

work page doi:10.1038/380603a0 1996
[22]

S. D. M. White and M. J. Rees, MNRAS183, 10.1093/mnras/183.3.341 (1978)

work page doi:10.1093/mnras/183.3.341 1978
[23]

Springel, MNRAS364, 1105 (2005), arXiv:astro- ph/0505010 [astro-ph]

V. Springel, MNRAS364, 1105 (2005), arXiv:astro- ph/0505010 [astro-ph]

work page arXiv 2005
[24]

Springel, Monthly notices of the royal astronomical society364, 1105 (2005)

V. Springel, Monthly notices of the royal astronomical society364, 1105 (2005)

2005
[25]

Zavala and C

J. Zavala and C. S. Frenk, Galaxies7, 81 (2019), arXiv:1907.11775 [astro-ph.CO]

work page arXiv 2019
[26]

A. G. Doroshkevich, Astrophysics6, 320 (1970)

1970
[27]

Y. B. Zel’dovich, A&A5, 84 (1970)

1970
[28]

S. F. Shandarin and Y. B. Zeldovich, Reviews of Modern Physics61, 185 (1989)

1989
[29]

Evolution of the cosmic web

M. Cautun, R. van de Weygaert, B. J. T. Jones, and C. S. Frenk, MNRAS441, 2923 (2014), arXiv:1401.7866 [astro-ph.CO]

work page Pith review arXiv 2014
[30]

N. I. Libeskind, R. van de Weygaert, M. Cautun, B. Falck, E. Tempel, T. Abel, M. Alpaslan, M. A. Aragón-Calvo, J.E.Forero-Romero, R.Gonzalez, S.Got- tlöber, O. Hahn, W. A. Hellwing, Y. Hoffman, B. J. Jones, F. Kitaura, A. Knebe, S. Manti, M. Neyrinck, S. E. Nuza, N. Padilla, E. Platen, N. Ramachandra, A. Robotham, E. Saar, S. Shandarin, M. Steinmetz, R. S...

2018
[31]

M. A. Aragón-Calvo, R. van de Weygaert, B. J. T. Jones, and J. M. van der Hulst, ApJ655, L5 (2007), arXiv:astro-ph/0610249 [astro-ph]

work page arXiv 2007
[32]

O. Hahn, C. M. Carollo, C. Porciani, and A. Dekel, MN- RAS381, 41 (2007), arXiv:0704.2595 [astro-ph]

work page arXiv 2007
[33]

and Hoffman, Yehuda and Crain, Robert A

O. Metuki, N. I. Libeskind, Y. Hoffman, R. A. Crain, and T. Theuns, MNRAS446, 10.1093/mnras/stu2166 (2015)

work page doi:10.1093/mnras/stu2166 2015
[34]

Alonso, E

D. Alonso, E. Eardley, and J. A. Peacock, MNRAS447, 2683 (2015), arXiv:1406.4159 [astro-ph.CO]

work page arXiv 2015
[35]

Ganeshaiah Veena, M

P. Ganeshaiah Veena, M. Cautun, R. van de Wey- gaert, E. Tempel, B. J. T. Jones, S. Rieder, and C. S. Frenk, MNRAS481, 414 (2018), arXiv:1805.00033 [astro-ph.CO]

work page arXiv 2018
[36]

W. A. Hellwing, M. Cautun, R. van de Weygaert, and B. T. Jones, Phys. Rev. D103, 063517 (2021), 15 arXiv:2011.08840 [astro-ph.CO]

work page arXiv 2021
[37]

Ganeshaiah Veena, M

P. Ganeshaiah Veena, M. Cautun, R. van de Weygaert, E. Tempel, and C. S. Frenk, MNRAS503, 2280 (2021), arXiv:2007.10365 [astro-ph.CO]

work page arXiv 2021
[38]

Moore, S

B. Moore, S. Ghigna, F. Governato, G. Lake, T. Quinn, J.Stadel,andP.Tozzi,ApJ524,L19(1999),arXiv:astro- ph/9907411 [astro-ph]

work page arXiv 1999
[39]

Klypin, A

A. Klypin, A. V. Kravtsov, O. Valenzuela, and F. Prada, ApJ522, 82 (1999), arXiv:astro-ph/9901240 [astro-ph]

work page arXiv 1999
[40]

Diemand, M

J. Diemand, M. Kuhlen, P. Madau, M. Zemp, B. Moore, D. Potter, and J. Stadel, Nature454, 735 (2008), arXiv:0805.1244 [astro-ph]

work page arXiv 2008
[41]

Springel, J

V. Springel, J. Wang, M. Vogelsberger, A. Ludlow, A. Jenkins, A. Helmi, J. F. Navarro, C. S. Frenk, and S. D. M. White, MNRAS391, 1685 (2008), arXiv:0809.0898 [astro-ph]

work page arXiv 2008
[42]

Ishiyama, F

T. Ishiyama, F. Prada, A. A. Klypin, M. Sinha, R. B. Metcalf, E. Jullo, B. Altieri, S. A. Cora, D. Croton, S. de la Torre, D. E. Millán-Calero, T. Oogi, J. Ruedas, and C. A. Vega-Martínez, MNRAS506, 4210 (2021), arXiv:2007.14720 [astro-ph.CO]

work page arXiv 2021
[43]

Hiroshima, S

N. Hiroshima, S. Ando, and T. Ishiyama, Phys. Rev. D 97, 123002 (2018), arXiv:1803.07691 [astro-ph.CO]

work page arXiv 2018
[44]

Boylan-Kolchin, J

M. Boylan-Kolchin, J. S. Bullock, and M. Kaplinghat, MNRAS415, L40 (2011), https://academic.oup.com/mnrasl/article- pdf/415/1/L40/54669362/mnrasl_415_1_l40.pdf

2011
[45]

L. E. Strigari and R. H. Wechsler, ApJ749, 75 (2012), arXiv:1111.2611 [astro-ph.CO]

work page arXiv 2012
[46]

F. C. van den Bosch and G. Ogiya, MNRAS475, 4066 (2018), arXiv:1801.05427 [astro-ph.GA]

work page arXiv 2018
[47]

S. B. Green, F. C. van den Bosch, and F. Jiang, MNRAS 503, 4075 (2021), arXiv:2103.01227 [astro-ph.GA]

work page arXiv 2021
[48]

L. E. Strigari, S. M. Koushiappas, J. S. Bullock, and M. Kaplinghat, Phys. Rev. D75, 083526 (2007), arXiv:astro-ph/0611925 [astro-ph]

work page arXiv 2007
[49]

Bergström, New Journal of Physics11, 105006 (2009), arXiv:0903.4849 [hep-ph]

L. Bergström, New Journal of Physics11, 105006 (2009), arXiv:0903.4849 [hep-ph]

work page arXiv 2009
[50]

Cirelli, Pramana79, 1021 (2012), arXiv:1202.1454 [hep-ph]

M. Cirelli, Pramana79, 1021 (2012), arXiv:1202.1454 [hep-ph]

work page arXiv 2012
[51]

Ishiyama and S

T. Ishiyama and S. Ando, MNRAS492, 3662 (2020), arXiv:1907.03642 [astro-ph.CO]

work page arXiv 2020
[52]

O. Hahn, C. Porciani, C. M. Carollo, and A. Dekel, MN- RAS375, 489 (2007), arXiv:astro-ph/0610280 [astro-ph]

work page arXiv 2007
[53]

Metuki, N

O. Metuki, N. I. Libeskind, and Y. Hoffman, MNRAS 460, 10.1093/mnras/stw979 (2016)

work page doi:10.1093/mnras/stw979 2016
[54]

Jiang and F

F. Jiang and F. C. V. D. Bosch, MNRAS458, 10.1093/mnras/stw439 (2016)

work page doi:10.1093/mnras/stw439 2016
[55]

Ogiya, O

G. Ogiya, O. Hahn, and A. B. Hirschmann, Monthly No- tices of the Royal Astronomical Society503, 1233 (2021)

2021
[56]

Errani and J

R. Errani and J. F. Navarro, Monthly Notices of the Royal Astronomical Society505, 18 (2021)

2021
[57]

Markos Hunde, O

F. Markos Hunde, O. Newton, W. A. Hellwing, M. Bilicki, and K. Naidoo, A&A700, A65 (2025), arXiv:2409.09226 [astro-ph.CO]

work page arXiv 2025
[58]

Moliné, M

Á. Moliné, M. A. Sánchez-Conde, A. Aguirre-Santaella, T. Ishiyama, F. Prada, S. A. Cora, D. Croton, E. Jullo, R. B. Metcalf, T. Oogi, and J. Ruedas, MNRAS518, 157 (2022)

2022
[59]

S. Bose, W. A. Hellwing, C. S. Frenk, A. Jenkins, M. R. Lovell, J. C. Helly, and B. Li, MNRAS455, 318 (2016)

2016
[60]

W. A. Hellwing, C. S. Frenk, M. Cautun, S. Bose, J. Helly, A. Jenkins, T. Sawala, and M. Cytowski, MN- RAS457, 3492 (2016), arXiv:1505.06436 [astro-ph.CO]

work page arXiv 2016
[61]

Cautun, R

M. Cautun, R. van de Weygaert, and B. J. T. Jones, MN- RAS429, 1286 (2013), arXiv:1209.2043 [astro-ph.CO]

work page arXiv 2013
[62]

M., Dunkley, J., et al

E. Komatsu, K. M. Smith, J. Dunkley, C. L. Bennett, B. Gold, G. Hinshaw, N. Jarosik, D. Larson, M. R. Nolta, L. Page, D. N. Spergel, M. Halpern, R. S. Hill, A. Kogut, M. Limon, S. S. Meyer, N. Odegard, G. S. Tucker, J. L. Weiland, E. Wollack, and E. L. Wright, ApJS192, 18 (2011), arXiv:1001.4538 [astro-ph.CO]

work page Pith review arXiv 2011
[63]

M.Davis, G.Efstathiou, C.S.Frenk,andS.D.M.White, ApJ292, 10.1086/163168 (1985)

work page doi:10.1086/163168 1985
[64]

Springel, S

V. Springel, S. D. M. White, G. Tormen, and G. Kauff- mann, MNRAS328, 726 (2001), arXiv:astro-ph/0012055 [astro-ph]

work page arXiv 2001
[65]

M. A. Aragón-Calvo, B. J. T. Jones, R. van de Wey- gaert, and J. M. van der Hulst, A&A474, 315 (2007), arXiv:0705.2072 [astro-ph]

work page arXiv 2007
[66]

Nurmi, P

P. Nurmi, P. Heinämäki, J. Holopainen, P. Pi- hajoki, E. Saar, M. Einasto, and J. Einasto, in Galaxy Evolution across the Hubble Time, Vol. 235, edited by F. Combes and J. Palouš (2007) pp. 127–127

2007
[67]

N. A. Bond, M. A. Strauss, and R. Cen, MNRAS409, 156 (2010), https://academic.oup.com/mnras/article- pdf/409/1/156/6221724/mnras0409-0156.pdf

2010
[68]

Hoffman, O

Y. Hoffman, O. Metuki, G. Yepes, S. Got- tlöber, J. E. Forero-Romero, N. I. Libe- skind, and A. Knebe, MNRAS425, 2049 (2012), https://academic.oup.com/mnras/article- pdf/425/3/2049/3052482/425-3-2049.pdf

2049
[69]

Pomarède, Y

D. Pomarède, Y. Hoffman, H. M. Courtois, and R. B. Tully, ApJ845, 55 (2017), arXiv:1706.03413 [astro- ph.CO]

work page arXiv 2017
[70]

J. E. Forero–Romero, Y. Hoffman, S. Gottlöber, A. Klypin, and G. Yepes, MNRAS396, 1815 (2009), https://academic.oup.com/mnras/article- pdf/396/3/1815/5804803/mnras0396-1815.pdf

2009
[71]

M. A. Aragón-Calvo, E. Platen, R. van de Weygaert, and A. S. Szalay, ApJ723, 364 (2010), arXiv:0809.5104 [astro-ph]

work page arXiv 2010
[72]

Sousbie, MNRAS414, 350 (2011), https://academic.oup.com/mnras/article- pdf/414/1/350/3809858/mnras0414-0350.pdf

T. Sousbie, MNRAS414, 350 (2011), https://academic.oup.com/mnras/article- pdf/414/1/350/3809858/mnras0414-0350.pdf

2011
[73]

Feldbrugge, R

J. Feldbrugge, R. van de Weygaert, J. Hidding, and J. Feldbrugge, J. Cosmology Astropart. Phys.2018, 027 (2018), arXiv:1703.09598 [astro-ph.CO]. [73]CaCTusis currently being prepared for public release and is not yet available at the time of writing

work page arXiv 2018
[74]

Cautun, S

M. Cautun, S. Bose, C. S. Frenk, Q. Guo, J. Han, W. A. Hellwing, T. Sawala, and W. Wang, MNRAS452, 3838 (2015), arXiv:1506.04151 [astro-ph.GA]

work page arXiv 2015
[75]

Kuhlen, J

M. Kuhlen, J. Diemand, and P. Madau, ApJ686, 262 (2008), arXiv:0805.4416 [astro-ph]

work page arXiv 2008
[76]

Stref, T

M. Stref, T. Lacroix, and J. Lavalle, Galaxies7, 65 (2019), arXiv:1905.02008 [astro-ph.CO]

work page arXiv 2019
[77]

Prada, A

F. Prada, A. A. Klypin, A. J. Cuesta, J. E. Betancort- Rijo, and J. Primack, MNRAS423, 3018 (2012), arXiv:1104.5130 [astro-ph.CO]

work page arXiv 2012
[78]

Avila-Reese, P

V. Avila-Reese, P. Colín, S. Gottlöber, C. Firmani, and C. Maulbetsch, ApJ634, 51 (2005), arXiv:astro- ph/0508053 [astro-ph]

work page arXiv 2005
[79]

Diemand, M

J. Diemand, M. Kuhlen, and P. Madau, ApJ667, 859 (2007), arXiv:astro-ph/0703337 [astro-ph]

work page arXiv 2007
[80]

J. E. Taylor and A. Babul, ApJ559, 716 (2001), arXiv:astro-ph/0012305 [astro-ph]

work page arXiv 2001

Showing first 80 references.