Constraining Cosmological Parameters Using the Splashback Radius of Galaxy Clusters

• DOI: 10.3847/1538-4357/ad5cee
• Publication Date: 2024-08-22T06:35:38Z
• Authors: Roan Haggar; Yuba Amoura; Charlie T. Mpetha; James E. Taylor; Kris Walker; Chris Power
• Keywords: Cosmological evolution; Cosmology and Nongalactic Astrophysics (astro-ph.CO); Cosmological parameters; FOS: Physical sciences; Galaxy clusters; Astrophysics; Astrophysics - Astrophysics of Galaxies; 01 natural sciences; QB460-466; Astrophysics of Galaxies (astro-ph.GA); 0103 physical sciences; N-body simulations; Astrophysics - Cosmology and Nongalactic Astrophysics

Abstract Cosmological parameters such as ΩM and σ 8 can be measured indirectly using various methods, including galaxy cluster abundance and cosmic shear. These measurements constrain the composite parameter S 8, leading to degeneracy between ΩM and σ 8. However, some structural properties of galaxy clusters also correlate with cosmological parameters, due to their dependence on a cluster’s accretion history. In this work, we focus on the splashback radius, an observable cluster feature that represents a boundary between a cluster and the surrounding Universe. Using a suite of cosmological simulations with a range of values for ΩM and σ 8, we show that the position of the splashback radius around cluster-mass halos is greater in cosmologies with smaller values of ΩM or larger values of σ 8. This variation breaks the degeneracy between ΩM and σ 8 that comes from measurements of the S 8 parameter. We also show that this variation is, in principle, measurable in observations. As the splashback radius can be determined from the same weak lensing analysis already used to estimate S 8, this new approach can tighten low-redshift constraints on cosmological parameters, either using existing data, or using upcoming data such as that from Euclid and LSST.