Abstract
The motivation of the present work is to reconstruct a dark energy model through the dimensionless dark energy functionX(z), which is the dark energy density in units of its present value. In this paper, we have shown that a scalar field phi having a phenomenologically chosen X(z) can give rise to a transition from a decelerated to an accelerated phase of expansion for the universe. We have examined the possibility of constraining various cosmological parameters (such as the deceleration parameter and the effective equation of state parameter) by comparing our theoretical model with the latest Type Ia Supernova (SN Ia), Baryon Acoustic Oscillations (BAO) and Cosmic Microwave Background (CMB) radiation observations. Using the joint analysis of the SN Ia+BAO/CMB dataset, we have also reconstructed the scalar potential from the parametrized X(z). The relevant potential is found, a polynomial in phi . From our analysis, it has been found that the present model favors the standard Lambda CDM model within 1sigma confidence level.
Highlights
In Ref. [30], Ellis and Madsen had discussed a reconstruction method to find the scalar field potential
We have focused on a quintessence model in which the scalar field is considered as a candidate of dark energy
We have constrained the model parameters using the SN Ia+Baryon Acoustic Oscillations (BAO)/Cosmic Microwave Background (CMB) (WMAP7) and SN Ia+BAO+CMB (Planck) datasets to study the different properties of this model extensively
Summary
In Ref. [30], Ellis and Madsen had discussed a reconstruction method to find the scalar field potential. [30], Ellis and Madsen had discussed a reconstruction method to find the scalar field potential. This method finds a very wide application in current research in cosmology. There are two types of reconstruction, namely, parametric and non-parametric.
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