Multiscale Cosmic Curvature: from Local Structures to Cosmology
David Benisty
TL;DR
The paper addresses how Dark Energy (DE) influences dynamics from local to cosmological scales by employing the McVittie spacetime to unify local gravity and cosmic expansion. It uses curvature invariants $\mathcal{R}$, $\mathcal{C}$, and $\mathcal{K}$ and introduces a universal dimensionless parameter $\kappa$ to compare regimes across galaxies, halos, and binaries, mapping these into a curvature phase space. The authors derive exact geodesic equations, present analytic expressions for the invariants, and demonstrate DE dominance near turnaround in groups and clusters, as well as in spherical density and binary systems, with validation from IllustrisTNG simulations and observational data. This geometric framework provides a scale-spanning diagnostic of DE effects, linking microphysical local dynamics to the large-scale cosmic acceleration and offering practical guidance for interpreting galaxy dynamics and structure formation in a $\Lambda$CDM context.
Abstract
This study tackles the impact Dark Energy (DE) in different systems by a simple unifying formalism. We introduce a parameter space that compare gravity across all cosmic scales, using the McVittie spacetime (McV) and connects spherically symmetric solutions with cosmological solutions. By analyzing the invariant scalars: the Ricci, Weyl, and Kretschmann scalars, we develop a phase-space description that predicts the dominance of the Cosmological Constant. We explore three cases: (1) the local Hubble flow around galaxy groups and clusters, (2) spherical density distributions and (3) binary motion. Our results show that the Kretschmann scalar of galaxy groups and clusters in their turnaround is $2Λ^2$ which is three times the Kretschmann scalar of the Cosmological Consonant. This quantifies the DE domination in local structures.
