2017/02/04 by Tomasz Denkiewicz, Vincenzo Salzano, Denkiewicz, Tomasz +1 · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #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)
paper · pdf · doi:10.48550/arxiv.1702.01291
openalex publication_date 2017/02/04 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
By means of the present geometrical and dynamical observational data, it is very hard to establish, from a statistical perspective, a clear preference among the vast majority of the proposed models for the dynamical dark energy and/or modified gravity theories alternative with respect to the ΛCDM scenario. On the other hand, on scales much smaller than present Hubble scale, there are possibly detectable differences in the growth of the matter perturbations for different modes of the perturbations, even in the context of the ΛCDM model. Here, we analyze the evolution of the dark matter perturbations in the context of ΛCDM and some dynamical dark energy models involving future cosmological singularities, such as the sudden future singularity and the finite scale factor singularity. We employ the Newtonian gauge formulation for the derivation of the perturbation equations for the growth function, and we abandon both the sub-Hubble approximation and the slowly varying potential assumption. We apply the Fisher Matrix approach to three future planned galaxy surveys e.g., DESI, Euclid, and WFirst-2.4. With the mentioned surveys on hand, only with the dynamical probes, we will achieve multiple goals: 1. the improvement in the accuracy of the determination of the fσ8 will give the possibility to discriminate between the ΛCDM and the alternative dark energy models even in the scale-independent approach; 2. it will be possible to test the goodness of the scale-independence finally, and also to quantify the necessity of a scale dependent approach to the growth of the perturbations, in particular using surveys which encompass redshift bins with scales k<0.005 h Mpc-1; 3. the scale-dependence itself might add much more discriminating power in general, but further advanced surveys will be needed.