Observational Constraints on Quintessence: Thawing, Tracker, and Scaling models

TL;DR

This paper uses recent cosmological data to constrain parameters of quintessence dark energy models, finding that some models are strongly limited and that the evolution of the universe closely resembles LCDM.

Contribution

It provides observational bounds on thawing, tracking, and scaling quintessence models using recent supernova, CMB, and BAO data, including BOSS.

Findings

Thawing models' w_0 constrained near -1 with BOSS data.

Tracker models with w_{(0)}<-0.949 are strongly favored.

Scaling models require early transition to w≈-1.

Abstract

For two types of quintessence models having thawing and tracking properties, there exist analytic solutions for the dark energy equation of state w expressed in terms of several free parameters. We put observational bounds on the parameters in such scenarios by using the recent data of Supernovae type Ia, Cosmic Microwave Background, and Baryon Acoustic Oscillations. The observational constraints are quite different depending on whether or not the recent BAO data from BOSS are taken into account. With the BOSS data the upper bounds of today's values of w (=w_0) in thawing models is very close to -1, whereas without this data the values of w_0 away from -1 can be still allowed. The tracker equation of state w_{(0)} during the matter era is constrained to be w_{(0)}<-0.949 at 95 % confidence level even without the BOSS data, so that the tracker models with w away from -1 are severely disfavored. We also study observational constraints on scaling models in which w starts to evolve from 0 in the deep matter era and show that the transition to the equation of state close to w=-1 needs to occur at an early cosmological epoch. In the three classes of quintessence models studied in this paper, the past evolution of the Hubble parameters in the best-fit models shows only less than the 2.5 % difference compared to the LCDM.