Cosmological implications and structure formation from a time varying vacuum

TL;DR

This paper investigates a cosmological model with a time-varying vacuum energy, analyzing its dynamics, observational constraints, and implications for structure formation, showing it predicts earlier galaxy cluster formation and faster perturbation growth.

Contribution

It introduces a $\Lambda(t)$ model with exponential functions for key cosmological variables and compares its predictions with standard $\Lambda$ cosmology using observational data.

Findings

$\Lambda(t)$ model fits supernova, CMB, and BAO data well.

Predicts earlier galaxy cluster formation compared to $\Lambda$ model.

Shows faster growth of perturbations in the $\Lambda(t)$ scenario.

Abstract

We study the dynamics of the FLRW flat cosmological models in which the vacuum energy varies with time, $\Lambda(t)$. In this model we find that the main cosmological functions such as the scale factor of the universe and the Hubble flow are defined in terms of exponential functions. Applying a joint likelihood analysis of the recent supernovae type Ia data, the Cosmic Microwave Background shift parameter and the Baryonic Acoustic Oscillations traced by the Sloan Digital Sky Survey (SDSS) galaxies, we place tight constraints on the main cosmological parameters of the $\Lambda(t)$ scenario. Also, we compare the $\Lambda(t)$ model with the traditional $\Lambda$ cosmology and we find that the former model provides a Hubble expansion which compares well with that of the $\Lambda$ cosmology. However, the $\Lambda(t)$ scenario predicts stronger small scale dynamics, which implies a faster growth rate of perturbations with respect to the usual $\Lambda$-cosmology, despite the fact that they share the same equation of state parameter. In this framework, we find that galaxy clusters in the $\Lambda(t)$ model appear to form earlier than in the $\Lambda$ model.