Cluster constraints on f (R) gravity

By F. Schmidt, A. Vikhlinin, Wayne Hu. 2009

190 citations recorded by the source corpus.

Modified gravitational forces in models that seek to explain cosmic acceleration without dark energy typically predict deviations in the abundance of massive dark matter halos. We conduct the first, simulation calibrated, cluster abundance constraints on a modified gravity model, specifically the modified action f(R) model. The local cluster abundance, when combined with geometric and high redshift data from the cosmic microwave background, supernovae, H0 and baryon acoustic oscillations, improve previous constraints by nearly 4 orders of magnitude in the field amplitude. These limits correspond to a 2 order of magnitude improvement in the bounds on the range of the force modification from the several Gpc scale to the tens of Mpc scale.

Subfields: Astronomy and Astrophysics, Oceanography

View Paper: https://www.semanticscholar.org/paper/60de885f9ab2742537187b38fd2a274f9091c514

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Citations in the corpus

Weighing the giants – IV. Cosmology and neutrino mass (2014, background): “…data have provided highly competitive constraints on dark energy and modifications of gravity (e.g. Vikhlinin et al. 2009; Mantz et al. 2010a; Schmidt et al. 2009; Rapetti et al. 2013), as well as measurements of the late-time normalization of the matter power spectrum (σ8, defined by…”
Weighing the Giants - I. Weak-lensing masses for 51 massive galaxy clusters: project overview, data analysis methods and cluster images (2012, background): “…of the most precise and robust constraints on dark energy (Vikhlinin et al. 2009b; Mantz et al. 2010a), as well as departures from General Relativity on cosmological scales (Rapetti et al. 2010, 2013; Schmidt et al. 2009), and the species-summed neutrino mass (Mantz et al. 2010c; Reid et al. 2010).”
f(R) Theories (2010, background): “See [530] for clustered abundance constraints on the f (R) model (4.”
Beyond the Cosmological Standard Model (2014, unknown): “The abundance of galaxy clusters from X-ray observations has been used to constrain the growth factor [909] and hence specific f(R) models [896].”
Modified Gravity and Cosmology (2011, methodology): “The matter power spectrum in f(R) theories of gravity has been considered in [495, 258, 1102, 122, 724, 1157, 790, 46, 45, 814, 1026], and cluster abundances have been used to constrain these theories in [1115, 818, 500].”
Testing gravity using cosmic voids (2014, background): “…choices of|fR0| are designed to cover the part of the parameter space which is cosmologically interes - ing: if |fR0| > 10−4 then thef(R) model violates the cluster abundance constraints (Schmidt et al. 2009), and if|fR0| < 10−6 then the model is too close toΛCDM to be distinguishable in cosmology.”
New observational constraints on f(R) gravity from cosmic chronometers (2016, methodology): “In the case of f(R) gravity such a confrontation with cosmological data was performed in [48] (using data from cosmic microwave background (CMB) probes), in [49, 50] (using Large Scale Structure (LSS) data), in [51] (using neutron stars mass-radius data), in [52] (using Supernovae type Ia (SNe Ia) a”
Formation of Galaxy Clusters (2012, methodology): “…obtained so far suggest that halo mass function and bias can still be described by the universal functions of peak height, in which the threshold for collapse and the linear growth rate are modified appropriately from their standard model values(Schmidt, Hu & Lima 2010; Schmidt et al. 2009).”
Cosmological Parameters from Observations of Galaxy Clusters (2011, background): “These include the self-accelerated branch (Chan & Scoccimarro 2009; Schmidt 2009b) and normal branch (Schmidt 2009a) of DGP gravity, and an f(R) model (Schmidt et al. 2009).”