2019/07/25 by Archita Bhattacharyya, Bhattacharyya, Archita, Supratik Pal +1
Physics and Astronomy · #Cosmology and Gravitation Theories #Cosmology and Nongalactic Astrophysics (astro-ph.CO) #Dark Matter and Cosmic Phenomena #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena
paper · pdf · doi:10.48550/arxiv.1907.10946
openalex publication_date 2019/07/25 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Dark Energy not only has background effects through its equation of state wDE, but also it can cluster through its sound speed c2sDE, subject to certain conditions. As is well-known, for dynamical dark energy models, dark energy perturbations get sourced into matter perturbations through metric perturbations which is always accompanied by the term (1+wDE). Hence, for dynamical dark energy models with wDE close -1, their perturbations get almost decoupled from metric leaving nearly null imprints on matter power spectra. Furthermore, Quintessence models with its sound speed equal to speed of light, washes out almost any inhomogeneities occurred within sub-Hubble scales, hence making detectability of dark energy perturbations far more difficult than already is. In this article we look for these imprints by going beyond Quintessence considering an Early Dark Energy parametrization that not only have a non-negligible energy density at early times, but also it can achieve wDE far from -1, making dark energy perturbations detectable in sub-horizon scales. With the help of current datasets, we are able to constrain sound speed of dark energy to a low value (c2sDE ∼ 0.14), along with a much higher range allowed for early dark energy density, with strong constraints on it (Ωe ∼ 0.02). We discuss effects of different datasets on this parametrization along with possible explanation for deviation on certain parameter(s) comparing between c2sDE=1 case and the case where it is kept open.