Nonlinear evolution of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>f</mml:mi><mml:mo stretchy="false">(</mml:mo><mml:mi>R</mml:mi><mml:mo stretchy="false">)</mml:mo></mml:math>cosmologies. II. Power spectrum

Oyaizu, Hiroaki; Lima, M.; Hu, Wayne

doi:10.1103/physrevd.78.123524

Cited by 214 publications

(286 citation statements)

References 46 publications

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“…Additionally, N-body simulations of gravitational collapse and clustering have been carried out in [393][394][395][396][397][398][399][400][401][402][403][404][405]. Functions of other curvature invariants have also been considered [406][407][408][409][410], but f (R) theories are distinguished in that they (and f (Gauss-Bonnet) theories) do not have ghosts.…”

Section: Example: F (R) Gravitymentioning

confidence: 99%

“…This affects various linear-scale observables [884,[902][903][904], such as enhanced large scale bulk flows [396,905], infall velocities [906] and weak-lensing signals [907] as described below. See [393][394][395][396][397][398][399][400][401][402][403][404] for N-body simulations.…”

Section: Astrophysical Tests Of Galileonsmentioning

confidence: 99%

“…For MG theories, the simulations incorporate the coupling of the density field to a scalar field such as f R for f (R) models. A number of papers have reported simulations that include such a coupling for both f (R) and DGP gravity [395,[395][396][397][398][1000][1001][1002].…”

Section: Halo Abundances and Profilesmentioning

confidence: 99%

“…Two essential products from simulations are the nonlinear mass power spectrum and the mass function of galaxy and cluster sized halos [395,397,398,[1000][1001][1002][1003]. For specific models these predictions allow for comparisons to data.…”

Section: Halo Abundances and Profilesmentioning

confidence: 99%

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Beyond the cosmological standard model

et al. 2015

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After a decade and a half of research motivated by the accelerating universe, theory and experiment have a reached a certain level of maturity. The development of theoretical models beyond Λ or smooth dark energy, often called modified gravity, has led to broader insights into a path forward, and a host of observational and experimental tests have been developed. In this review we present the current state of the field and describe a framework for anticipating developments in the next decade. We identify the guiding principles for rigorous and consistent modifications of the standard model, and discuss the prospects for empirical tests.We begin by reviewing recent attempts to consistently modify Einstein gravity in the infrared, focusing on the notion that additional degrees of freedom introduced by the modification must "screen" themselves from local tests of gravity. We categorize screening mechanisms into three broad classes: mechanisms which become active in regions of high Newtonian potential, those in which first derivatives of the field become important, and those for which second derivatives of the field are important. Examples of the first class, such as f (R) gravity, employ the familiar chameleon or symmetron mechanisms, whereas examples of the last class are galileon and massive gravity theories, employing the Vainshtein mechanism. In each case, we describe the theories as effective theories and discuss prospects for completion in a more fundamental theory. We describe experimental tests of each class of theories, summarizing laboratory and solar system tests and describing in some detail astrophysical and cosmological tests. Finally, we discuss prospects for future tests which will be sensitive to different signatures of new physics in the gravitational sector.The review is structured so that those parts that are more relevant to theorists vs. observers/experimentalists are clearly indicated, in the hope that this will serve as a useful reference for both audiences, as well as helping those interested in bridging the gap between them.

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Section: Example: F (R) Gravitymentioning

confidence: 99%

Section: Astrophysical Tests Of Galileonsmentioning

confidence: 99%

Section: Halo Abundances and Profilesmentioning

confidence: 99%

Section: Halo Abundances and Profilesmentioning

confidence: 99%

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Beyond the cosmological standard model

et al. 2015

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“…In order for this scenario to work, gravity must be significantly modified from General Relativity (GR) on cosmological scales, but has to reduce to GR locally in order to satisfy stringent Solar System constraints at a few AU. Thus, a working modified gravity model has to include a non-linear mechanism to restore GR in high-density environments, which can have a noticeable impact on the formation of large-scale structure on intermediate scales of a few to tens of Mpc [6][7][8][9].…”

Section: Introductionmentioning

confidence: 99%

Spherical collapse and the halo model in braneworld gravity

2010

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We present a detailed study of the collapse of a spherical perturbation in DGP braneworld gravity for the purpose of modeling simulation results for the halo mass function, bias and matter power spectrum. The presence of evolving modifications to the gravitational force in form of the scalar brane-bending mode lead to qualitative differences to the collapse in ordinary gravity. In particular, differences in the energetics of the collapse necessitate a new, generalized method for defining the virial radius which does not rely on strict energy conservation. These differences and techniques apply to smooth dark energy models with w = −1 as well. We also discuss the impact of the exterior of the perturbation on collapse quantities due to the lack of a Birkhoff theorem in DGP. The resulting predictions for the mass function, halo bias and power spectrum are in good overall agreement with DGP N-body simulations on both the self-accelerating and normal branch. In particular, the impact of the Vainshtein mechanism as measured in the full simulations is matched well. The model and techniques introduced here can serve as practical tools for placing consistent constraints on braneworld models using observations of large scale structure.

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Constraining chameleon models with cosmology

2014

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Chameleon fields may modify gravity on cluster scales while recovering general relativity locally. This article reviews signatures of chameleon modifications in the nonlinear cosmological structure, comparing different techniques to model them, summarising the current state of observational constraints, and concluding with an outlook on prospective constraints from future observations and applications of the analytic tools developed in the process to more general scalar-tensor theories. Particular focus is given to the Hu-Sawicki and designer models of f (R) gravity.

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Nonlinear evolution off(R)cosmologies. II. Power spectrum

Cited by 214 publications

References 46 publications

Beyond the cosmological standard model

Beyond the cosmological standard model

Spherical collapse and the halo model in braneworld gravity

Constraining chameleon models with cosmology

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