AIC and BIC for cosmological interacting scenarios

Arevalo, Fabiola; Cid, Antonella; Moya, Jorge Viteri

doi:10.1140/epjc/s10052-017-5128-7

Cited by 53 publications

(53 citation statements)

References 63 publications

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“…The effect of the new term redefines the coefficients in the sign-changeable interaction Q, thus we obtain a new Q q that has the same form of the sign-changeable interaction (6).…”

Section: Solvable Sign-changeable Interaction Scenariomentioning

confidence: 99%

“…Interactions Q(ρ, ρ ) In the left column, we present five sign-changeable interactions investigated in the literature that involve the deceleration parameter q while in the right, we write these interactions in terms of ρ and ρ according to (6). Here, α i , α and β are interaction parameters.…”

Section: Interacting Dark Sector With Sign-changeable Interactionmentioning

confidence: 99%

“…Finally, we comment that the initial interaction proportional to a quadratic polynomial on q can be enlarged by including a term proportional to the first η-derivative of the deceleration parameter Q q ∝ ρq . This generates an additional term in the sign-changeable interaction (6), so that it takes the new form Q q = Q + s 4 ρ , with s 4 an arbitrary constant. However, it is easy to see that the new term s 4 ρ modifies the coefficient of ρ in the source equation (10), so that ρ → (1 − s 4 ∆)ρ , then we solve for…”

Section: Solvable Sign-changeable Interaction Scenariomentioning

confidence: 99%

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On sign-changeable interaction in FLRW cosmology

et al. 2019

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We investigate an interacting two-fluid model in a spatially flat Friedmann-Lemaître-Robertson-Walker (FLRW) Universe, when the energy transfer between these two dark components is produced by a factorisable nonlinear sign-changeable interaction depending linearly on the energy density and quadratically on the deceleration parameter. We solve the source equation and obtain the effective energy densities of the dark sector and their components. We show that the effective equation of state of the dark sector includes some of the several kind of Chaplygin gas equations of state as well as a generalization of the polytropic equation of state. We use bayesian statistics methods to constrain free parameters in the models during its most recent evolution considering supernovae type Ia and measurements of the Hubble expansion rate. The resulting constraints provide new information on sign-changeable interactions, its equivalences and compatibility with previous models and novel late time universe

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“…The effect of the new term redefines the coefficients in the sign-changeable interaction Q, thus we obtain a new Q q that has the same form of the sign-changeable interaction (6).…”

Section: Solvable Sign-changeable Interaction Scenariomentioning

confidence: 99%

Section: Interacting Dark Sector With Sign-changeable Interactionmentioning

confidence: 99%

Section: Solvable Sign-changeable Interaction Scenariomentioning

confidence: 99%

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On sign-changeable interaction in FLRW cosmology

et al. 2019

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“…In particular, interacting models of dark energy and dark matter [4][5][6][7][8] are based on the premise that no known symmetry in Nature prevents or suppresses a non-minimal coupling between these components and, therefore, such possibility must be investigated in light of observational data 1 (for a recent review, see [9]). In some classes of these coupled models the coincidence problem above mentioned can be largely alleviated when compared with the standard cosmology.…”

Section: Introductionmentioning

confidence: 99%

“…Since then, a number of interacting models with both numerical and analytical solutions have been proposed (see, e.g. [6][7][8][10][11][12][13][14][15][16] and references therein).…”

Section: Introductionmentioning

confidence: 99%

Bayesian comparison of interacting scenarios

Cid

Santos

Pigozzo

et al. 2019

J. Cosmol. Astropart. Phys.

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We perform a Bayesian model selection analysis for different classes of phenomenological coupled scenarios of dark matter and dark energy with linear and non-linear interacting terms. We use a combination of some of the latest cosmological data such as type Ia supernovae (SNe Ia), cosmic chronometers (CC), cosmic microwave background (CMB) and two sets of baryon acoustic oscillations measurements, namely, 2-dimensional angular measurements (BAO2) and 3-dimensional angle-averaged measurements (BAO3). We find weak and moderate evidence against two-thirds of the interacting scenarios considered with respect to ΛCDM when the full joint analysis is considered. About one-third of the models provide a description to the data as good as the one provided by the standard model. Our results also indicate that either SNe Ia, CC or BAO2 data by themselves are not able to distinguish among interacting models or ΛCDM but the standard BAO3 measurements and the combination with the CMB data are indeed able to discriminate among them. We find that evidence disfavoring interacting models is weaker when we use BAO2 (data claimed to be almost model-independent) instead of the standard BAO3 measurements. These results help select classes of viable and non-viable interacting models in light of current data.

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Observational constraints on the free parameters of an interacting Bose–Einstein gas as a dark-energy model

2018

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Dark energy is modelled by a Bose-Einstein gas of particles with an attractive interaction. It is coupled to cold dark matter, within a flat universe, for the late-expansion description, producing variations in particle-number densities. The model's parameters, and physical association, are: Ω G0 , Ω m0 , the darkenergy rest-mass energy density and the dark-matter term scaling as a mass term, respectively; Ω i0 , the self-interaction intensity; x, the energy exchange rate. Energy conservation relates such parameters. The Hubble equation omits Ω G0 , but also contains h, the present-day expansion rate of the flat Friedman-Lemâitre-Robertson-Walker metric, and Ω b0 , the baryon energy density, used as a prior. This results in the four effective chosen parameters Ω b0 , h, Ω m0 , Ω i0 , fit with the Hubble expansion rate H(z), and data from its value today, near distance, and supernovas. We derive wide 1σ and 2σ likelihood regions compatible with definite positive total CDM and IBEG mass terms. Additionally, the best-fit value of parameter x relieves the coincidence problem, and a second potential coincidence problem related to the choice of Ω

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AIC and BIC for cosmological interacting scenarios

Cited by 53 publications

References 63 publications

On sign-changeable interaction in FLRW cosmology

On sign-changeable interaction in FLRW cosmology

Bayesian comparison of interacting scenarios

Observational constraints on the free parameters of an interacting Bose–Einstein gas as a dark-energy model

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