A Bayesian comparison between $$\Lambda $$CDM and phenomenologically emergent dark energy models

Rezaei, Mehdi; Naderi, Tayebe; Malekjani, M.; Mehrabi, Ahmad

doi:10.1140/epjc/s10052-020-7942-6

Cited by 55 publications

(36 citation statements)

References 69 publications

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“…The very same model has been updated in reference [394], which finds H 0 = 72.35 +0.78 −0.79 km s −1 Mpc −1 at 68% CL for the Planck 2018 data, and H 0 = 72.16 ± 0.44 km s −1 Mpc −1 at 68% CL for Planck 2018 + CMB lensing + BAO + Pantheon + DES + R19, confirming the agreement with R20 within one standard deviation. However, in reference [395] it has been argued that, while at the background level the flat-PEDE model fits the data as well as the ΛCDM scenario, at the perturbation level the PEDE model cannot fit the observational data in cluster scales compared to the ΛCDM. Extensions of this model considering neutrinos or a non-zero curvature of the Universe can be found in references [394][395][396].…”

Section: Phenomenologically Emergent Dark Energymentioning

confidence: 99%

In the realm of the Hubble tension—a review of solutions ^*

Valentino

Mena²,

Pan³

et al. 2021

Class. Quantum Grav.

1,414

760

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The simplest ΛCDM model provides a good fit to a large span of cosmological data but harbors large areas of phenomenology and ignorance. With the improvement of the number and the accuracy of observations, discrepancies among key cosmological parameters of the model have emerged. The most statistically significant tension is the 4σ to 6σ disagreement between predictions of the Hubble constant, H 0, made by the early time probes in concert with the ‘vanilla’ ΛCDM cosmological model, and a number of late time, model-independent determinations of H 0 from local measurements of distances and redshifts. The high precision and consistency of the data at both ends present strong challenges to the possible solution space and demands a hypothesis with enough rigor to explain multiple observations—whether these invoke new physics, unexpected large-scale structures or multiple, unrelated errors. A thorough review of the problem including a discussion of recent Hubble constant estimates and a summary of the proposed theoretical solutions is presented here. We include more than 1000 references, indicating that the interest in this area has grown considerably just during the last few years. We classify the many proposals to resolve the tension in these categories: early dark energy, late dark energy, dark energy models with 6 degrees of freedom and their extensions, models with extra relativistic degrees of freedom, models with extra interactions, unified cosmologies, modified gravity, inflationary models, modified recombination history, physics of the critical phenomena, and alternative proposals. Some are formally successful, improving the fit to the data in light of their additional degrees of freedom, restoring agreement within 1–2σ between Planck 2018, using the cosmic microwave background power spectra data, baryon acoustic oscillations, Pantheon SN data, and R20, the latest SH0ES Team Riess, et al (2021 Astrophys. J. 908 L6) measurement of the Hubble constant (H 0 = 73.2 ± 1.3 km s−1 Mpc−1 at 68% confidence level). However, there are many more unsuccessful models which leave the discrepancy well above the 3σ disagreement level. In many cases, reduced tension comes not simply from a change in the value of H 0 but also due to an increase in its uncertainty due to degeneracy with additional physics, complicating the picture and pointing to the need for additional probes. While no specific proposal makes a strong case for being highly likely or far better than all others, solutions involving early or dynamical dark energy, neutrino interactions, interacting cosmologies, primordial magnetic fields, and modified gravity provide the best options until a better alternative comes along.

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Section: Phenomenologically Emergent Dark Energymentioning

confidence: 99%

In the realm of the Hubble tension—a review of solutions ^*

Valentino

Mena²,

Pan³

et al. 2021

Class. Quantum Grav.

1,414

760

View full text Add to dashboard Cite

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“…(Di Valentino 2020c;Di Valentino et al 2021;Perivolaropoulos & Skara 2021) and references therein. Some of these models have good consistency with different observations while some others have been ruled out after comparing with observational data (see also Malekjani et al 2017;Malekjani et al 2018;Lusso et al 2019;Rezaei 2019a,b;Lin et al 2019;Rezaei, Malekjani & Solà 2019;Rezaei et al 2020aRezaei et al , 2021. Therefore, cosmologists felt motivated to propose different scenarios in which the origin of DE is based on more physical principles and ultimately on fundamental theory.…”

Section: Introductionmentioning

confidence: 99%

Cosmographic approach to Running Vacuum dark energy models: new constraints using BAOs and Hubble diagrams at higher redshifts

Rezaei,

Sola,

Malekjani

2021

Preprint

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In this work we study different types of dark energy (DE) models in the framework of the cosmographic approach, with emphasis on the Running Vacuum models (RVMs). We assess their viability using different information criteria and compare them with the so-called Ghost DE models (GDEs) as well as with the concordance ΛCDM model. We use the Hubble diagrams for Pantheon SnIa, quasars (QSOs), gamma-ray bursts (GRBs) as well as the data on baryonic acoustic oscillations (BAOs) in four different combinations. Upon minimizing the χ 2 function of the distance modulus in the context of the Markov Chain Monte Carlo method (MCMC), we put constraints on the current values of the standard cosmographic parameters in a model-independent way. It turns out that, in the absence of BAOs data, the various DE models generally exhibit cosmographic tensions with the observations at the highest redshifts (namely with the QSOs and GRBs data). However, if we include the robust observations from BAOs to our cosmographic sample, the ΛCDM and RVMs are clearly favored against the GDEs. Finally, judging from the perspective of the deviance information criterion (DIC), which enables us to compare models making use of the Markov chains of the MCMC method, we conclude that the RVMs are the preferred kind of DE models. We find it remarkable that these models, which had been previously shown to be capable of alleviating the σ 8 and H 0 tensions, appear now also as the most successful ones at the level of the cosmographic analysis.

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“…There are many approaches in order to investigate the DE, e.g., the dynamical DE, phantom DE, quintessence, Chaplygin gas, holographic DE, the interaction between DE and DM, phenomenological emergent DE, and early DE (see Refs. [18,[20][21][22][23][24][25][26][27][28]). Among several models to investigate the DE, the thermodynamic approach has been widely investigated (see, e.g., Refs.…”

Section: Introductionmentioning

confidence: 99%

Growth of matter perturbations in the extended viscous dark energy models

Silva

2021

Eur. Phys. J. C

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In this work, we study the extended viscous dark energy models in the context of matter perturbations. To do this, we assume an alternative interpretation of the flat Friedmann–Lemaître–Robertson–Walker Universe, through the nonadditive entropy and the viscous dark energy. We implement the relativistic equations to obtain the growth of matter fluctuations for a smooth version of dark energy. As result, we show that the matter density contrast evolves similarly to the $$\Lambda $$ Λ CDM model in high redshift; however, in late time, it is slightly different from the standard model. Using the latest geometrical and growth rate observational data, we carry out a Bayesian analysis to constrain parameters and compare models. We see that our viscous models are compatible with cosmological probes, and the $$\Lambda $$ Λ CDM recovered with a $$1\sigma $$ 1 σ confidence level. The viscous dark energy models relieve the tension of $$H_0$$ H 0 in $$2 \sim 3 \sigma $$ 2 ∼ 3 σ . Yet, by involving the $$\sigma _8$$ σ 8 tension, some models can alleviate it. In the model selection framework, the data discards the extended viscous dark energy models.

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A Bayesian comparison between $$\Lambda $$CDM and phenomenologically emergent dark energy models

Cited by 55 publications

References 69 publications

In the realm of the Hubble tension—a review of solutions ^*

In the realm of the Hubble tension—a review of solutions ^*

Cosmographic approach to Running Vacuum dark energy models: new constraints using BAOs and Hubble diagrams at higher redshifts

Growth of matter perturbations in the extended viscous dark energy models

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A Bayesian comparison between $$\Lambda $$CDM and phenomenologically emergent dark energy models

Cited by 55 publications

References 69 publications

In the realm of the Hubble tension—a review of solutions *

In the realm of the Hubble tension—a review of solutions *

Cosmographic approach to Running Vacuum dark energy models: new constraints using BAOs and Hubble diagrams at higher redshifts

Growth of matter perturbations in the extended viscous dark energy models

Contact Info

Product

Resources

About

In the realm of the Hubble tension—a review of solutions ^*

In the realm of the Hubble tension—a review of solutions ^*