Cluster abundance in<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>gravity models

Ferraro, Simone; Schmidt, Fabian; Hu, Wayne

doi:10.1103/physrevd.83.063503

Cited by 108 publications

(117 citation statements)

References 31 publications

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“…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%

“…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%

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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: Astrophysical Tests Of Galileonsmentioning

confidence: 99%

Section: Example: F (R) Gravitymentioning

confidence: 99%

Beyond the cosmological standard model

et al. 2015

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“…The parameters for the f (R) and the symmetron models are summarised in Table 1. In the case of the f (R)-gravity, the parameter n was fixed to one, while f R0 took values from 10 −6 , which resulted in hardly any deviation from ΛCDM, to 10 −4 , which is on the border of violating cluster abundance constraints (Ferraro et al 2011). For the symmetron model mainly the time of the symmetry breaking was varied while leaving the others constant except for one of the model that also has an increased coupling constant.…”

Section: The Simulationsmentioning

confidence: 99%

Gravitational redshift profiles in thef(R)and symmetron models

Grönke

Llinares

Mota

2014

A&A

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Aims. We investigate the gravitational redshift in clusters of galaxies in the symmetron and Hu-Sawicky f (R) models. The characteristic feature of both models is the screening mechanism that hides the fifth force in dense environments recovering general relativity. Methods. We use N-body simulations that were run with the code Isis, which includes scalar fields, to analyse the deviation of observables in modified gravity models with respect to ΛCDM. Results. We find that the presence of the screening makes the deviation highly dependent on the halo mass. For instance, the f (R) parameters | f R0 | = 10 −5 , n = 1 cause an enhancement of the gravitational signal by up to 50% for haloes with masses between 10 13 M h −1 and 10 14 M h −1 . The characteristic mass range where the fifth force is most active varies with the model parameters. The usual assumption is that the presence of a fifth force leads to a deeper potential well and thus a stronger gravitational redshift. However, we find that in cases in which only the central regions of the haloes are screened, there could also be a weaker gravitational redshift.

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“…However, unlike Rapetti et al (2011), Ferraro et al (2011, Cataneo et al (2014), we use cluster profiles, rather than abundances to do so. The hypothesis is that a fifth force would be screened in the dense cluster cores, but not in the rarefied cluster outskirts (Burikham & Panpanich 2012, Lombriser et al 2012.…”

mentioning

confidence: 99%

“…On megaparsec and larger scales, Raveri et al (2014) used the Cosmic Microwave Background to measure |fR0|< 10 −3 . Also on large scales Rapetti et al (2011), Ferraro et al (2011, Cataneo et al (2014) used the abundance of galaxy clusters to constrain |fR0|, e.g. Cataneo et al (2014) measured (under the assumption of n = 1), |fR0|< 2.6 × 10 −5 .…”

mentioning

confidence: 99%

TheXMMCluster Survey: testing chameleon gravity using the profiles of clusters

Wilcox¹,

Bacon²,

Nichol³

et al. 2015

Mon. Not. R. Astron. Soc.

106

116

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The chameleon gravity model postulates the existence of a scalar field that couples with matter to mediate a fifth force. If it exists, this fifth force would influence the hot X-ray emitting gas filling the potential wells of galaxy clusters. However, it would not influence the clusters weak lensing signal. Therefore, by comparing X-ray and weak lensing profiles, one can place upper limits on the strength of a fifth force. This technique has been attempted before using a single, nearby cluster (Coma, z = 0.02, Terukina et al. 2014). Here we apply the technique to the stacked profiles of 58 clusters at higher redshifts (0.1 < z < 1.2 ), including 12 new to the literature, using X-ray data from the XMM Cluster Survey (XCS) and weak lensing data from the Canada France Hawaii Telescope Lensing Survey (CFHTLenS). Using a multiparameter MCMC analysis, we constrain the two chameleon gravity parameters (β and φ ∞ ). Our fits are consistent with general relativity, not requiring a fifth force. In the special case of f (R) gravity (where β = 1/6), we set an upper limit on the background field amplitude today of |f R0 |< 6 × 10 −5 (95% CL). This is one of the strongest constraints to date on |f R0 | on cosmological scales. We hope to improve this constraint in future by extending the study to hundreds of clusters using data from the Dark Energy Survey.

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Cluster abundance inf(R)gravity models

Cited by 108 publications

References 31 publications

Beyond the cosmological standard model

Beyond the cosmological standard model

Gravitational redshift profiles in thef(R)and symmetron models

TheXMMCluster Survey: testing chameleon gravity using the profiles of clusters

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