Abstract
We investigate the role played by dark energy perturbations in the skewness ${S}_{3}$ of large-scale matter distribution. We consider a two-fluid universe composed by matter and dark energy, with perturbations in both components, and we estimate numerically the skewness of the matter density field as a function of the dark energy parameters. We characterize today's ${S}_{3}$ value for quintessence and phantom dark energy cosmologies as well as its dependence on the matter density parameter ${\mathrm{\ensuremath{\Omega}}}_{m0}$ and the dark energy sound speed ${c}_{s}^{2}$ with accurate numerical fitting. These fits can be used to test cosmology against future high quality data on large scale structure.
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