Generalized tracker quintessence models for dark energy

Ureña–López, L. Arturo; Roy, Nandan

doi:10.1103/physrevd.102.063510

Cited by 39 publications

(14 citation statements)

References 53 publications

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“…Although the percentage deviation is not much, but one should, in principle, take into account the dark energy perturbations as well to obtain the complete picture. A similar claim has been made in [69] that if one does not consider the dark energy perturbations, this can result in misleading constraints on the cosmological parameters.…”

Section: A Observational Constraintssupporting

confidence: 55%

Quintessence or Phantom: Study of scalar field dark energy models through a general parametrization of the Hubble parameter

Roy¹,

Goswami²,

Das³

2022

Preprint

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In this work we propose a simple general parametrization scheme of the Hubble parameter for the scalar field dark energy models. In our approach it is possible to incorporate both the quintessence and phantom scalar field in a single analytical scheme and write down relevant cosmological parameters which are independent of the nature of the scalar field. A general condition for the phantom barrier crossing has also been obtained. To test this approach, a well behaved parametrization of the normalized Hubble parameter has been considered and a wide variety of observational data like CMB data, Supernovae data, BAO data etc. has been used to constraint the various cosmological parameters. It has been found that data prefer the present value of the equation of state of the dark energy to be in the phantom domain. One interesting outcome of this analysis is that although the current value of the dark energy equation of state is phantom in nature, a phantom crossing of the EOS has taken place in the recent past. We have also carried out the Bayesian model comparison between ΛCDM model and the proposed model which indicates that this model is favored by data as compared to ΛCDM model.

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Section: A Observational Constraintssupporting

confidence: 55%

Quintessence or Phantom: Study of scalar field dark energy models through a general parametrization of the Hubble parameter

Roy¹,

Goswami²,

Das³

2022

Preprint

Self Cite

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“…For recent studies on constraints on φCDM see Refs. [88][89][90][91][92][93][94][95][96][97][98][99][100][101] and related references within these papers.…”

Section: Cosmological Modelsmentioning

confidence: 99%

$H_0=69.8\pm1.3$ $\rm{km \ s^{-1} \ Mpc^{-1}}$, $Ω_{m0}=0.288\pm0.017$, and other constraints from lower-redshift, non-CMB and non-distance-ladder, expansion-rate data

Cao¹,

Ratra²

2023

Preprint

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We use updated Type Ia Pantheon+ supernova, baryon acoustic oscillation, and Hubble parameter (now also accounting for correlations) data, as well as new reverberation-measured C iv quasar data, and quasar angular size, H ii starburst galaxy, reverberation-measured Mg ii quasar, and Amaticorrelated gamma-ray burst data to constrain cosmological parameters. We show that these data sets result in mutually consistent constraints and jointly use them to constrain cosmological parameters in six different spatially-flat and non-flat cosmological models. Our analysis provides summary modelindependent determinations of two key cosmological parameters: the Hubble constant, H0 = 69.8 ± 1.3 km s −1 Mpc −1 , and the current non-relativistic matter density parameter, Ωm0 = 0.288 ± 0.017. Our summary error bars are 2.4 and 2.3 times those obtained using the flat ΛCDM model and Planck TT,TE,EE+lowE+lensing cosmic microwave background (CMB) anisotropy data. Our H0 value is very consistent with that from the local expansion rate based on the Tip of the Red Giant Branch data, is 2σ lower than that from the local expansion rate based on Type Ia supernova and Cepheid data, and is 2σ higher than that in the flat ΛCDM model based on Planck TT,TE,EE+lowE+lensing CMB data. Our data compilation shows at most mild evidence for non-flat spatial hypersurfaces, but more significant evidence for dark energy dynamics, 2σ or larger in the spatially-flat dynamical dark energy models we study.

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“…As we explain in Sect. 5, the perturbations to the scalar field also play a crucial role in driving the parameter inferences, and as such it is both theoretically and practically inconsistent to disregard the perturbations as is done in [40] and as the authors themselves point out in [41] (the implications of inconsistently accounting for the scalar field perturbations was first noted in [42]). The specific model we study here contributes significantly to the energy density prior to recombination, but less so after and appears to represent a best-case scenario for a single, minimally coupled scalar field with fairly generic initial conditions in alleviating the value of H 0 inferred from Planck.…”

Section: Cosmological Tensions and Attempts At Resolutionmentioning

confidence: 99%

Quintessential Cosmological Tensions

Adil¹,

Albrecht²,

Knox³

2022

Preprint

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Several cosmological tensions have emerged in light of recent data, most notably in the inferences of the parameters H0 and σ8. We explore the possibility of alleviating both these tensions simultaneously by means of the Albrecht-Skordis "quintessence" potential. The field can reduce the size of the sound horizon r * s while concurrently suppressing the power in matter density fluctuations before it comes to dominate the energy density budget today. Interestingly, this rich set of dynamics is governed entirely by one free parameter that is of O(10) in Planck units. We find that the inferred value of H0 can be increased, while that of σ8 can be decreased, both by ≈ 1σ compared to the ΛCDM case. However, ultimately the model is disfavored by Planck and BAO data alone, compared to the standard ΛCDM model, with a ∆χ 2 ≈ +6. When including large scale structure and supernova data ∆χ 2 ≈ +1. We note that historically much attention has been focused on preserving the three angular scales θD, θEQ, and θ * s to their ΛCDM values. Our work presents an example of how, while doing so indeed maintains a relatively good fit to the CMB data for an increased number of ultra-relativistic species, it is a-priori insufficient in maintaining such a fit in more general model spaces.

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Generalized tracker quintessence models for dark energy

Cited by 39 publications

References 53 publications

Quintessence or Phantom: Study of scalar field dark energy models through a general parametrization of the Hubble parameter

Quintessence or Phantom: Study of scalar field dark energy models through a general parametrization of the Hubble parameter

$H_0=69.8\pm1.3$ $\rm{km \ s^{-1} \ Mpc^{-1}}$, $Ω_{m0}=0.288\pm0.017$, and other constraints from lower-redshift, non-CMB and non-distance-ladder, expansion-rate data

Quintessential Cosmological Tensions

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