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Halo model and halo properties in Galileon gravity cosmologies
Cosmology and Nongalactic Astrophysics · Submitted 7 Jan 2014
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The nonlinear matter power spectrum computed in the halo model approach is found to be inaccurate in the mildly nonlinear regime, but captures reasonably well the effects of the Vainshtein screening mechanism on small scales.
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The abstract, sentence by sentence
We investigate the performance of semi-analytical modelling of large-scale structure in Galileon gravity cosmologies using results from N-body simulations. We focus on the Cubic and Quartic Galileon models that provide a reasonable fit to CMB, SNIa and BAO data. We demonstrate that the Sheth-Tormen mass function and linear halo bias can be calibrated to provide a very good fit to our simulation results. We also find that the halo concentration-mass relation is well fitted by a power law. The nonlinear matter power spectrum computed in the halo model approach is found to be inaccurate in the mildly nonlinear regime, but captures reasonably well the effects of the Vainshtein screening mechanism on small scales. In the Cubic model, the screening mechanism hides essentially all of the effects of the fifth force inside haloes. In the case of the Quartic model, the screening mechanism leaves behind residual modifications to gravity, which make the effective gravitational strength time-varying and smaller than the standard value. Compared to normal gravity, this causes a deficiency of massive haloes and leads to a weaker matter clustering on small scales. For both models, we show that there are realistic halo occupation distributions of Luminous Red Galaxies that can match both the observed large-scale clustering amplitude and the number density of these galaxies.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We investigate the performance of semi-analytical modelling of large-scale structure in Galileon gravity cosmologies using results from N-body simulations. | contribution 0.94 | 0.94 | 0.05 | asserted 0.52 |
| s1 | We focus on the Cubic and Quartic Galileon models that provide a reasonable fit to CMB, SNIa and BAO data. | background 0.36 | 0.23 | 0.03 | asserted 0.88 |
| s2 | We demonstrate that the Sheth-Tormen mass function and linear halo bias can be calibrated to provide a very good fit to our simulation results. | result 0.97 | 0.95 | 0.22 | asserted 1.00 |
| s3 | We also find that the halo concentration-mass relation is well fitted by a power law. | result 1.00 | 0.94 | 0.07 | asserted 1.00 |
| s4 | The nonlinear matter power spectrum computed in the halo model approach is found to be inaccurate in the mildly nonlinear regime, but captures reasonably well the effects of the Vainshtein screening mechanism on small scales. | result 0.98 | 0.95 | 0.24 | asserted 1.00 |
| s5 | In the Cubic model, the screening mechanism hides essentially all of the effects of the fifth force inside haloes. | result 0.90 | 0.88 | 0.10 | asserted 1.00 |
| s6 | In the case of the Quartic model, the screening mechanism leaves behind residual modifications to gravity, which make the effective gravitational strength time-varying and smaller than the standard value. | result 0.92 | 0.90 | 0.13 | asserted 1.00 |
| s7 | Compared to normal gravity, this causes a deficiency of massive haloes and leads to a weaker matter clustering on small scales. | interpretation 0.59 | 0.86 | 0.13 | asserted 1.00 |
| s8 | For both models, we show that there are realistic halo occupation distributions of Luminous Red Galaxies that can match both the observed large-scale clustering amplitude and the number density of these galaxies. | result 0.99 | 0.92 | 0.16 | asserted 0.93 |
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The paper
Original abstract
We investigate the performance of semi-analytical modelling of large-scale structure in Galileon gravity cosmologies using results from N-body simulations. We focus on the Cubic and Quartic Galileon models that provide a reasonable fit to CMB, SNIa and BAO data. We demonstrate that the Sheth-Tormen mass function and linear halo bias can be calibrated to provide a very good fit to our simulation results. We also find that the halo concentration-mass relation is well fitted by a power law. The nonlinear matter power spectrum computed in the halo model approach is found to be inaccurate in the mildly nonlinear regime, but captures reasonably well the effects of the Vainshtein screening mechanism on small scales. In the Cubic model, the screening mechanism hides essentially all of the effects of the fifth force inside haloes. In the case of the Quartic model, the screening mechanism leaves behind residual modifications to gravity, which make the effective gravitational strength time-varying and smaller than the standard value. Compared to normal gravity, this causes a deficiency of massive haloes and leads to a weaker matter clustering on small scales. For both models, we show that there are realistic halo occupation distributions of Luminous Red Galaxies that can match both the observed large-scale clustering amplitude and the number density of these galaxies.
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References
How the literature uses it
24 arXiv papers cite this in 55 sentences
Papers citing it · 36 sentences without a confident label
Uses its method or tool 3 papers
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We model all these quantities in the remainder of this section, in which we follow the notation of Refs. [ref] .
Nonlinear structure formation in Nonlocal Gravity · Halo model · 0.86
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These two quantities were evaluated by following the strategy presented in Refs. [ref] .
The observational status of Galileon gravity after Planck · Local time variation of $G_eff$ in the Quartic model · 1.00
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Our strategy follows closely that presented in Refs. [ref] , to which we refer the interested reader for more details.
Validating estimates of the growth rate of structure with modified gravity simulations · Best-fitting Sheth-Tormen mass function · 1.00
Compares with it 3 papers
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The concentration-mass relation of the CLASH clusters for the three models is shown in Fig. [ref], together with results from N-body simulations [ref] .
Galaxy cluster lensing masses in modified lensing potentials · Cluster lensing masses in Galileon and Nonlocal gravity · 0.86
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The fifth force enhances the abundance of dark matter haloes in the entire mass range probed by the simulations, with the enhancement stronger at late times and for high-mass haloes, which mimics the effect of the csG model [ref] .
Proca-stinated Cosmology II: Matter, Halo, and Lensing Statistics in the vector Galileon · Halo mass function · 0.81
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There are still some visible discrepancies at $a = 0.60$, which are similar to those found in Ref. [ref] for Galileon gravity models.
Nonlinear structure formation in Nonlocal Gravity · Nonlinear matter power spectrum · 1.00
Cites it as background 10 papers
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Next we summarise the key expressions of the halo model (see [ref] for a comprehensive review) in general theories of gravity [ref] .
Modelling the matter bispectrum at small scales in modified gravity · Halo model · 0.92
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For later stages of structure formation, the picture becomes more complex due to the nonlinearities of the screening mechanism [ref] .
$\nu$Galileon: modified gravity with massive neutrinos as a testable alternative to $\Lambda$CDM · Background · 0.82
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The HM formalism has been used to model non-linear MG PS in [ref] , which is mainly based on the theoretical spherical collapse model, and is explicitly solved for each MG variant.
Improved analytical modeling of the non-linear power spectrum in modified gravity cosmologies · Introduction · 0.87
What it cites · 109 sentences without a confident label
Contests 4 papers
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This conclusion is contrary to the concerns raised in Refs. [ref] .
The parameter space in Galileon gravity models · Halo occupation distribution analysis · contest 0.76
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This conclusion is contrary to the concerns raised in Refs. [ref] .
Linear perturbations in Galileon gravity models · Halo occupation distribution analysis · contest 0.76
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This conclusion is contrary to the concerns raised in Refs. [ref] .
Spherical collapse in Galileon gravity: fifth force solutions, halo mass function and halo bias · Halo occupation distribution analysis · contest 0.76
Builds on 1 paper
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Here, our goal is to put the excursion set theory predictions of Ref. [ref] on to a more quantitative level.
Spherical collapse in Galileon gravity: fifth force solutions, halo mass function and halo bias · Introduction · 0.97
Uses the method or tool of 9 papers
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Ultimately, we use these halo properties to determine the nonlinear matter power spectrum computed in the halo model approach [ref] .
Halo Models of Large Scale Structure · Introduction · 0.96
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We follow the notation of Ref. [ref] , to which we refer the reader for further details of the derivation.
Spherical collapse in Galileon gravity: fifth force solutions, halo mass function and halo bias · Halo model · 0.85
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The simulations presented in this paper were performed with the ECOSMOG code [ref] , which is a modified version of the RAMSES code [ref] that includes extra solvers for the scalar degrees of freedom that appear in modified gravity theories.
Cosmological Hydrodynamics with Adaptive Mesh Refinement: a new high resolution code called RAMSES · Summary of the simulations · 1.00
Uses data or values from 2 papers
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For the Cubic and Quartic Galileon models, we have that $f_Cubic ≈f_Quartic ≈0.75$ and $R_Cubic ≈R_Quartic ≈1.10$ (see Fig. 1 of Ref. [ref] ).
Spherical collapse in Galileon gravity: fifth force solutions, halo mass function and halo bias · Halo occupation distribution analysis · 0.97
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We take $n̅_g = 4 ×10^-5 h^3/Mpc^3$, which corresponds roughly to $∫n(z) dz$, where $n(z)$ is the redshift dependence of the observed galaxy number density (see Fig. 1 of Ref. [ref] ).
Cosmological Constraints from the Clustering of the Sloan Digital Sky Survey DR7 Luminous Red Galaxies · Halo occupation distribution analysis · 1.00
Compares with 5 papers
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This overestimation is similar to that found in Ref. [ref] for Dvali-Gabadadze-Porrati (DGP) models and Refs. [ref] for $f(R)$ models of gravity.
Non-linear Evolution of f(R) Cosmologies III: Halo Statistics · Halo model matter power spectrum · 1.00
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This overestimation is similar to that found in Ref. [ref] for Dvali-Gabadadze-Porrati (DGP) models and Refs. [ref] for $f(R)$ models of gravity.
Spherical Collapse and the Halo Model in Braneworld Gravity · Halo model matter power spectrum · 1.00
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This overestimation is similar to that found in Ref. [ref] for Dvali-Gabadadze-Porrati (DGP) models and Refs. [ref] for $f(R)$ models of gravity.
Halo modelling in chameleon theories · Halo model matter power spectrum · 1.00
Cites as support 2 papers
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The screening mechanism could potentially suppress part of the enhancement, but Refs. [ref] have shown that the impact of the Vainshtein effect is negligible on sufficiently large scales ($k ≲0.1 h/Mpc$).
Nonlinear structure formation in the Cubic Galileon gravity model · Halo occupation distribution analysis · 0.97
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The screening mechanism could potentially suppress part of the enhancement, but Refs. [ref] have shown that the impact of the Vainshtein effect is negligible on sufficiently large scales ($k ≲0.1 h/Mpc$).
Simulating the quartic Galileon gravity model on adaptively refined meshes · Halo occupation distribution analysis · 0.97
Cites as background 22 papers
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References [ref] and [ref] performed the first N-body simulations of the covariant Galileon model of Ref. [ref] .
Simulating the quartic Galileon gravity model on adaptively refined meshes · Introduction · 0.96
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References [ref] and [ref] performed the first N-body simulations of the covariant Galileon model of Ref. [ref] .
Nonlinear structure formation in the Cubic Galileon gravity model · Introduction · 0.96
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This is a mechanism that is widely known as the Vainshtein effect [ref] .
Effective theory for the Vainshtein mechanism from the Horndeski action · Introduction · 0.94
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