AIC, BIC, Bayesian evidence against the interacting dark energy model

Szydłowski, Marek; Krawiec, Adam; Kurek, Aleksandra; Kamionka, Michał

doi:10.1140/epjc/s10052-014-3236-1

Cited by 42 publications

(28 citation statements)

References 79 publications

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“…This is consistent with the results of Ref. [31], where the authors conclude that the particular interacting model they study is disfavored compared to CDM, also they notice that BIC is a more restrictive criteria. The model ωCDM is also incompatible with CDM with respect to BIC.…”

Section: Analysis and Resultssupporting

confidence: 92%

AIC and BIC for cosmological interacting scenarios

2017

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In this work we study linear and nonlinear cosmological interactions, which depend on dark matter and dark energy densities in the framework of general relativity. By using the Akaike information criterion (AIC) and the bayesian information criterion (BIC) with data from SnIa (Union 2.1 and binned JLA), H(z), BAO and CMB we compare the interacting models among themselves and analyze whether more complex interacting models are favored by these criteria. In this context, we find some suitable interactions that alleviate the coincidence problem.

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Section: Analysis and Resultssupporting

confidence: 92%

AIC and BIC for cosmological interacting scenarios

2017

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“…From Table 3 the Jeffreys scale applied to the AIC statistical criterion favors the model RRG+RGE, while this model is strongly disfavored using the BIC criterium, a consequence of the large number of observational data, specially the SNIa data. This discrepancy in using the two criteria is a common feature found in the literature [54][55][56]. The contourplots with 1σ and 2σ Fig.…”

Section: Including Bao and Snia Datamentioning

confidence: 68%

Primordial universe with the running cosmological constant

et al. 2020

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Theoretically, the running of the cosmological constant in the IR region is not ruled out. On the other hand, from the QFT viewpoint, the energy released due to the variation of the cosmological constant in the late Universe cannot go to the matter sector. For this reason, the phenomenological bounds on such a running are not sufficiently restrictive. The situation can be different in the early Universe when the gravitational field was sufficiently strong to provide an efficient creation of particles from the vacuum. We develop a framework for systematically exploring this possibility. It is supposed that the running occurs in the epoch when the Dark Matter already decoupled and is expanding adiabatically, while the usual matter should be regarded approximately massless and can be abundantly created from vacuum due to the decay of vacuum energy. By using the handy model of Reduced Relativistic Gas for describing the warm Dark Matter, we consider the dynamics of both cosmic background and linear perturbations and evaluate the impact of the vacuum decay on the matter power spectrum and to the first CMB peak. Additionally, using the combined SNIa+BAO data, we find the best-fit values for the free parameters of the model.

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“…We use the Akaike Information Criterion (AIC) and the Bayesian Information Criterion (BIC). For details see [51,52,53] AIC = χ 2 + 2P BIC = χ 2 + 2P lnd where P and d are the number of model parameters and data points in the dataset respectively. χ 2 is the minimum value of chi square.…”

Section: Information Criteriamentioning

confidence: 99%

Transition redshift: new constraints from parametric and nonparametric methods

Rani

Jain

Mahajan

et al. 2015

J. Cosmol. Astropart. Phys.

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In this paper, we use the cosmokinematics approach to study the accelerated expansion of the Universe. This is a model independent approach and depends only on the assumption that the Universe is homogeneous and isotropic and is described by the FRW metric. We parametrize the deceleration parameter, q(z), to constrain the transition redshift (z t ) at which the expansion of the Universe goes from a decelerating to an accelerating phase. We use three different parametrizations of q(z) namely, q I (z) = q 1 + q 2 z, q II (z) = q 3 + q 4 ln(1 + z) and q III (z) = 1 2 + q 5 (1+z) 2 . A joint analysis of the age of galaxies, strong lensing and supernovae Ia data indicates that the transition redshift is less than unity i.e. z t < 1. We also use a nonparametric approach (LOESS+SIMEX) to constrain z t . This too gives z t < 1 which is consistent with the value obtained by the parametric approach.

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AIC, BIC, Bayesian evidence against the interacting dark energy model

Cited by 42 publications

References 79 publications

AIC and BIC for cosmological interacting scenarios

AIC and BIC for cosmological interacting scenarios

Primordial universe with the running cosmological constant

Transition redshift: new constraints from parametric and nonparametric methods

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