Cluster Constraints on f(R) Gravity
arXiv:0908.2457 · doi:10.1103/PhysRevD.80.083505
Abstract
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, H_0 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.
9 pages, 7 figures; v2: minor revisions, matches version accepted for publication in Phys. Rev. D
References in corpus (11)
- Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation
- New Hubble Space Telescope Discoveries of Type Ia Supernovae at z > 1: Narrowing Constraints on the Early Behavior of Dark Energy
- Models of f(R) Cosmic Acceleration that Evade Solar-System Tests
- Disappearing cosmological constant in f(R) gravity
- Observational Constraints on the Nature of the Dark Energy: First Cosmological Results from the ESSENCE Supernova Survey
- Non-linear Evolution of f(R) Cosmologies III: Halo Statistics
- Non-linear evolution of f(R) cosmologies II: power spectrum
- Non-linear evolution of f(R) cosmologies I: methodology
- Cosmological Constraints on f(R) Acceleration Models
- N-Body Simulations of DGP and Degravitation Theories
- Exploring the Energetics of Intracluster Gas with a Simple and Accurate Model