Limits on the Reconstruction of a Single Dark Energy Scalar Field Potential from SNe Ia Data

Piloyan, Arpine; Pavluchenko, Sergey A.; Amendola, Luca

doi:10.3390/particles1010003

Cited by 13 publications

(3 citation statements)

References 56 publications

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“…Te transition redshift determined in [146] and in [147] from the "Supernova Legacy Survey (SNLS)" is z t ∼ 0.6 (1; σ), which is more consistent with the fat Λ CDM model (z t � (2Ω Λ /Ω m ) 1/3 − 1 ∼ 0.66, joint analysis) [148] is an extra limitation. In addition, the transition redshift we determined for our model is z t ≈ 0.752,1.758 for two observed data sets (see Figure 5), which is in good agreement with the Hubble diagram of SNe Ia, including the SNI997f at z t ≈ 1.7 [123,149]. Tis fnding suggests in a roundabout way that the history of cosmic expansion can be revised using the transition redshift.…”

supporting

confidence: 83%

LRS Bianchi Type-I String Cosmological Models in $f (Q)$ Gravity

Kumar

Singh²,

Bajaj

et al. 2023

Journal of Mathematics

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In the current study, we studied a f Q -gravitational, anisotropic, locally rotationally symmetric (LRS), Bianchi type-I spacetime universe. We have adopted the freely chosen function f Q = Q + α Q , where α is a model-free parameter. We assumed that the universe is filled with dusty string fluid and that the shear scalar ( σ ) and the expansion scalar ( θ ) are proportional to each other in order to solve field equations for the average Hubble parameter ( H ). The resultant Hubble function has been fitted with observational datasets H z and SNe Ia datasets of apparent magnitude m z in order to obtain the best fit values for the cosmological parameters. Utilizing these best fit values throughout the analysis, many cosmic phenomena are examined. We have investigated cosmographic coefficients such as H , q , j , a n d s to see if an accelerated transit phase dark energy model of the cosmos exists. Also, we have classified the dark energy models that are explored using Om diagnostic analysis; our universe model is a quintessential dark energy model. The age of the universe as it exists right now has been roughly calculated by the model.

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supporting

confidence: 83%

LRS Bianchi Type-I String Cosmological Models in $f (Q)$ Gravity

Kumar

Singh²,

Bajaj

et al. 2023

Journal of Mathematics

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“…With the GP method, one can reconstruct a general function of the model directly from data, without the need of a particular parameterization for it. The reconstruction of a DE scalar field potential was done in [36,37] and limits from SNe Ia data was obtained recently by [38]. There are several other recent analysis of cosmological parameters reconstructed through GP method.…”

Section: Jcap11(2022)037mentioning

confidence: 99%

Gaussian processes reconstruction of the dark energy potential

Jesus

Valentim

Escobal

et al. 2022

J. Cosmol. Astropart. Phys.

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Scalar Fields (SF) have emerged as natural candidates for dark energy as quintessential or phantom fields, as they are the main ingredient of inflation theories. Instead of assuming some form for the scalar field potential, however, this work reconstructs the SF potential directly from observational data, namely, Hubble and SNe Ia data. We show that two popular forms for the SF potentials, namely, the power-law and the quadratic free-field, are compatible with the reconstructions thus obtained, at least for some choices of the priors of the matter density and curvature parameters and for some redshift intervals.

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“…A line of approach is the reconstruction of the scalar field potential in a manner consistent with the SNe Ia data. The article by A. Piloyan et al [12] suggests a method of reconstruction of this potential and concludes that the accuracy of the current data is insufficient for such a reconstruction.…”

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confidence: 99%