Generalized holographic cosmology: low-redshift observational constraint (original) (raw)
Related papers
Generalized holographic cosmology
Classical and Quantum Gravity, 2013
We consider general black hole solutions in five-dimensional spacetime in the presence of a negative cosmological constant. We obtain a cosmological evolution via the gravity/gauge theory duality (holography) by defining appropriate boundary conditions on a four-dimensional boundary hypersurface. The standard counterterms are shown to renormalize the bare parameters of the system (the four-dimensional Newton's constant and cosmological constant). We discuss the thermodynamics of cosmological evolution and present various examples. The standard braneworld scenarios are shown to be special cases of our holographic construction. †
Dark Energy Constraints from a five-dimensional AdS Black Hole via AdS/CFT
EPJ Web of Conferences
There are many dark energy models having been investigated with constraint from observational data. The best dark energy candidate is ΛCDM model. In this work, our model has extended to include AdS/CFT correspondent, where the AdS black hole boundary exhibit the FLRW metric foliated with four-dimensional gravity theory, can lead to a modified Friedmann Equation contains extra parameter coming from 5D AdS (hairy) black hole, where such extension to ACDM can be considered. We obtained modified Friedmann equation from both 5D hairless and scalar hair black hole. The effect from extra dimension in hairless black hole solutions can be observed in the form of radiation. Also, it is interesting to see a non-trivial term emerges in scalar hair solution case. However in this study, we only consider Hairless black hole case for data constraint by using a join analysis of Supernovae, CMB and H0 measurement to obtain $ \chi _{\min }^2 $ . As a result, we compare this particular case with ACDM us...
Features of holographic dark energy under combined cosmological constraints
The European Physical Journal C, 2009
We investigate the observational signatures of the holographic dark energy models in this paper, including both the original model and a model with an interaction term between the dark energy and dark matter. We first delineate the dynamical behavior of such models, especially whether they would have "Big Rip" for different parameters, then we use several recent observations, including 182 highquality type Ia supernovae data observed with the Hubble Space Telescope, the SNLS and ESSENCE surveys, 42 latest Chandra X-ray cluster gas mass fraction, 27 high-redshift gamma-ray burst samples, the baryon acoustic oscillation measurement from the Sloan Digital Sky Survey, and the CMB shift parameter from WMAP three years result to give more reliable and tighter constraints on the holographic dark energy models. The results of our constraints for the holographic dark energy model without interaction is c = 0.748 +0.108 −0.009 , Ω m0 = 0.276 +0.017 −0.016 , and for model with interaction (c = 0.692 +0.135 −0.107 , Ω m0 = 0.281 +0.017 −0.017 ,α = −0.006 +0.021 −0.024 , where α is an interacting parameter). As these models have more parameters than the ΛCDM model, we use the Bayesian evidence as a model selection criterion to make comparison. We found that the holographic dark energy models are mildly favored by the observations compared with the ΛCDM model.
The European Physical Journal C
The cosmography method is a model-independent technique used to reconstruct the Hubble expansion of the Universe at low redshifts. In this method, using the Hubble diagrams from Type Ia Supernovae (SNIa) in Pantheon catalog, quasars and Gamma-Ray Bursts (GRB), we put observational constraints on the cosmographic parameters in holographic dark energy (HDE) and concordance \varLambda ΛCDMmodelsbyminimizingtheerrorfunctionΛ CDM models by minimizing the error functionΛCDMmodelsbyminimizingtheerrorfunction\chi ^2$$ χ 2 based on the statistical Markov Chain Monte Carlo (MCMC) algorithm. Then, we compare the results of the models with the results of the model-independent cosmography method. Except for the Pantheon sample, we observe that there is a big tension between standard cosmology and Hubble diagram observations, while the HDE model remains consistent in all cases. Then we use different combinations of Hubble diagram data to reconstruct the Hubble parameter of the model and compare it with the observed Hubble data. We observe that the Hubble paramete...
A 5D holographic dark energy in DGP-BRANE cosmology
Astrophysics and Space Science, 2014
This paper is aimed at investigating a 5D holographic dark energy in DGP-BRANE cosmology by employing a combination of Sne Ia, BAO and CMB observational data to fit the cosmological parameters in the model. We describe the dynamic of a FRW for the normal branch (ǫ = +1) of solutions of the induced gravity brane-world model. We take the matter in 5D bulk as holographic dark energy that its holographic nature is reproduced effectively in 4D. The cosmic evolution reveals that the effective 4D holographic dark energy behaves as quintessence while taking into account the 4D cold dark matter results in matter dominated universe followed by late time acceleration.
Observational constraints on the cosmology with holographic dark fluid
Physics of the Dark Universe, 2021
We consider the holographic Friedman-Robertson-Walker (hFRW) universe on the 4dimensional membrane embedded in the 5-dimensional bulk spacetime, and fit the parameters with the observational data. In order to fully account for the phenomenology of this scenario, we consider the models with the brane cosmological constant and the negative bulk
INJE-TP-01-04, hep-th/0104159 Holographic principle in the BDL brane cosmology
2001
We study the holographic principle in the brane cosmology. Especially we describe how to accommodate the 5D anti de Sitter Schwarzschild (AdSS5) black hole in the Binetruy-Deffayet-Langlois (BDL) approach of brane cosmology. It is easy to make a connection between a mass M of the AdSS5 black hole and a conformal field theory (CFT)-radiation dominated universe on the brane in the moving domain wall approach. But this is not established in the BDL approach. In this case we use two parameters C1,C2 in the Friedmann equation. These arise from integration and are really related to the choice of initial bulk matter. If one chooses a bulk energy density ρB to account for a mass M of the AdSS5 black hole and the static fifth dimension, a CFTradiation term with ρCFT ∼ M/a 4 comes out from the bulk matter without introducing a localized matter distribution on the brane. This means that the holographic principle can be established in the BDL brane cosmology.
Holographic dark-energy models
Physical Review D, 2011
Different holographic dark-energy models are studied from a unifying point of view. We compare models for which the Hubble scale, the future event horizon or a quantity proportional to the Ricci scale are taken as the infrared cutoff length. We demonstrate that the mere definition of the holographic dark-energy density generally implies an interaction with the dark-matter component. We discuss the relation between the equation-of-state parameter and the energy density ratio of both components for each of the choices, as well as the possibility of non-interacting and scaling solutions. Parameter estimations for all three cutoff options are performed with the help of a Bayesian statistical analysis, using data from supernovae type Ia and the history of the Hubble parameter. The ΛCDM model is the clear winner of the analysis. According to the Bayesian Information Criterion (BIC), all holographic models should be considered as ruled out, since the difference ∆BIC to the corresponding ΛCDM value is > 10. According to the Akaike Information Criterion (AIC), however, we find ∆AIC < 2 for models with Hubble-scale and Ricci-scale cutoffs, indicating, that they may still be competitive. As we show for the example of the Ricci-scale case, also the use of certain priors, reducing the number of free parameters to that of the ΛCDM model, may result in a competitive holographic model.