Chameleon Screening Depends on the Shape and Structure of NFW Halos
arXiv:2108.10364 · doi:10.1088/1475-7516/2022/04/047
Abstract
Chameleon gravity is an example of a model that gives rise to interesting phenomenology on cosmological scales while simultaneously possessing a screening mechanism, allowing it to avoid solar system constraints. Such models result in non-linear field equations, which can be solved analytically only in simple highly symmetric systems. In this work we study the equation of motion of a scalar-tensor theory with chameleon screening using the finite element method. More specifically, we solve the field equation for spherical and triaxial NFW cluster-sized halos. This allows a detailed investigation of the relationship between the NFW concentration and the virial mass parameters and the magnitude of the chameleon acceleration, as measured at the virial radius. In addition, we investigate the effects on the chameleon acceleration due to halo triaxiality. We focus on the parameter space regions that are still allowed by the observational constraints. We find that given our dataset, the largest allowed value for the chameleon-to-NFW acceleration ratio at the virial radius is . This result strongly indicates that the chameleon models that are still allowed by the observational constraints would not lead to any measurable effects on galaxy cluster scales. Nonetheless, we also find that there is a direct relationship between the NFW potential and the chameleon-to-NFW acceleration ratio at the virial radius. Similarly, there is a direct (yet a much more complicated) relationship between the NFW concentration, the virial mass and the acceleration ratios at the virial radius. Finally, we find that triaxiality introduces extra directional effects on the acceleration measurements. These effects in combination could potentially be used in future observational searches for fifth forces.
arXiv comment32 pages, 21 figures, 1 table, submitted to JCAP
References in corpus (48)
- XGBoost: A Scalable Tree Boosting System
- A Universal Density Profile from Hierarchical Clustering
- Dynamics of dark energy
- A direct empirical proof of the existence of dark matter
- Chameleon Cosmology
- MultiDark simulations: the story of dark matter halo concentrations and density profiles
- Ahf: Amiga's Halo Finder
- Triaxial Modeling of Halo Density Profiles with High-resolution N-body Simulations
- DOLFIN: Automated Finite Element Computing
- Cosmological Tests of Modified Gravity
- The evolution substructure I: a new identification method
- Tests of Chameleon Gravity
- Symmetron Cosmology
- Clusters of galaxies with modified Newtonian dynamics (MOND)
- Cool Core Clusters from Cosmological Simulations
- Astrophysical Tests of Modified Gravity: Constraints from Distance Indicators in the Nearby Universe
- Experiment to detect dark energy forces using atom interferometry
- Segue 2: The Least Massive Galaxy
- No-Go Theorems for Generalized Chameleon Field Theories
- Testing gravity with cold atom interferometry: Results and prospects
- Probing Dark Energy with Atom Interferometry
- New observational constraints on gravity from cosmic chronometers
- A Compendium of Chameleon Constraints
- Cluster Density Profiles as a Test of Modified Gravity
- The Three-Dimensional Shapes of Galaxy Clusters
- Testing chameleon gravity with the Coma cluster
- Chameleon Dark Energy and Atom Interferometry
- Constraining chameleon models with cosmology
- The XMM Cluster Survey: Testing chameleon gravity using the profiles of clusters
- Testing Gravity Using Galaxy Clusters: New Constraints on Beyond Horndeski Theories
- Dark energy interactions near the galactic centre
- Hydrostatic and Caustic Mass Profiles of Galaxy Clusters
- A general framework to test gravity using galaxy clusters II: A universal model for the halo concentration in gravity
- Simulation tests of galaxy cluster constraints on chameleon gravity
- Imprints of Chameleon f(R) Gravity on Galaxy Rotation Curves
- Tests of Gravity with Galaxy Clusters
- The Three Hundred Project: Substructure in hydrodynamical and dark matter simulations of galaxy groups around clusters
- The shape dependence of chameleon screening
- Zoomed cosmological simulations of Milky Way sized halos in f(R)-gravity
- Triaxial vs. Spherical Dark Matter Halo Profiles
- SELCIE: A tool for investigating the chameleon field of arbitrary sources
- Cosmic structures from a mathematical perspective 1. Dark matter halo mass density profiles
- Constraints on chameleon gravity from the measurement of the electrostatic stiffness of the MICROSCOPE mission accelerometers
- Modeling the formation of galaxy clusters in MOND
- Testing Emergent Gravity on Galaxy Cluster Scales
- Fifth-Force Screening around Extremely Compact Sources
- enics: Vainshtein screening with the finite element method
- Density Profile of a Cool Core of Galaxy Clusters