2023/09/13 by Xiaoyun Shao, Shao, Xiaoyun, Rodrigo S. Gonçalves +9 · 3 citations
Physics and Astronomy · #Cosmology and Gravitation Theories #Cosmology and Nongalactic Astrophysics (astro-ph.CO) #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #General Relativity and Quantum Cosmology (gr-qc) #Scientific Research and Discoveries
paper · pdf · doi:10.48550/arxiv.2309.07263
openalex publication_date 2023/09/13 · openalex created_date 2023/09/16 · openalex updated_date 2026/08/01
In standard cosmology, the cosmic homogeneity scale is the transition scale above which the patterns arising from non-uniformities -- such as groups and clusters of galaxies, voids, and filaments -- become indistinguishable from a random distribution of sources. Recently, different groups have investigated the feasibility of using such a scale as a cosmological test and arrived at different conclusions. In this paper, we complement and extend these studies by exploring the evolution of the spatial (\calRH) and angular (θH) homogeneity scales with redshift, assuming a spatially flat, Λ-Cold Dark Matter %(ΛCDM) universe and linear cosmological perturbation theory. We confirm previous results concerning the non-monotonicity of \calRH with the matter density parameter Ωm0 but also show that it exhibits a monotonical behavior with the Hubble constant H0 within a large redshift interval. More importantly, we find that, for z \gtrsim 0.6, the angular homogeneity scale not only presents a monotonical behavior with Ωm0 and H0 but is quite sensitive to H0, especially at higher redshifts. These results, therefore, raise the possibility of using θH as a new, model-independent way to constrain cosmological parameters.