Constraints on holographic dark energy from the latest supernovae, galaxy clustering, and cosmic microwave background anisotropy observations

Zhang, Jingfei; Wu, Fengquan

doi:10.1103/physrevd.76.023502

Cited by 204 publications

(48 citation statements)

References 86 publications

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“…The number of works devoted to the Holographic Dark Energy Models, beginning from the first publication [28], is ever growing [31][32][33][34][35][36][37][38][39][40][41][42][43][44][45][46][47][48] to relieve us of citing the whole list.…”

Section: Holographic Dark Energy Modelsmentioning

confidence: 99%

Entropy in the Present and Early Universe: New Small Parameters and Dark Energy Problem

Shalyt-Margolin

2010

Entropy

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It is demonstrated that entropy and its density play a significant role in solving the problem of the vacuum energy density (cosmological constant) of the Universe and hence the dark energy problem. Taking this in mind, two most popular models for dark energy-Holographic Dark Energy Model and Agegraphic Dark Energy Model-are analysed. It is shown that the fundamental quantities in the first of these models may be expressed in terms of a new small dimensionless parameter that is naturally occurring in High Energy Gravitational Thermodynamics and Gravitational Holography (UV-limit). On this basis, the possibility of a new approach to the problem of Quantum Gravity is discussed. Besides, the results obtained on the uncertainty relation of the pair "cosmological constant-volume of space-time", where the cosmological constant is a dynamic quantity, are reconsidered and generalized up to the Generalized Uncertainty Relation.

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Section: Holographic Dark Energy Modelsmentioning

confidence: 99%

Entropy in the Present and Early Universe: New Small Parameters and Dark Energy Problem

Shalyt-Margolin

2010

Entropy

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“…The HDE model has been widely studied in depth [33][34][35][36][37][38][39][40][41][42][43][44][45][46][47][48][49][50][51][52].…”

Section: Introductionmentioning

confidence: 99%

Reexploration of interacting holographic dark energy model: cases of interaction term excluding the Hubble parameter

Zhang

Lü

et al. 2017

Eur. Phys. J. C

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In this paper, we make a deep analysis for the five typical interacting holographic dark energy models with the interaction terms, respectively. We obtain observational constraints on these models by using the type Ia supernova data (the Joint LightCurve Analysis sample), the cosmic microwave background data (Planck 2015 distance priors), the baryon acoustic oscillations data, and the direct measurement of the Hubble constant. We find that the values of χ 2 min for all the five models are almost equal (around 699), indicating that the current observational data equally favor these IHDE models. In addition, a comparison with the cases of an interaction term involving the Hubble parameter H is also made.

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“…[17,19] the vacuum zero-point energy ρ X is considered as holographic dark energy, and the largest L allowed is the one saturating this inequality, thus…”

mentioning

confidence: 99%

“…However, in the HDE model [17,19], the equation of state will cross −1 when the parameter c is taken to be less than 1. Moreover, the observations show that the parameter c is indeed less than one [19].…”

mentioning

confidence: 99%

Modified Chaplygin gas as an interacting holographic dark energy model

Yang

Wang

et al. 2010

Sci. China Phys. Mech. Astron.

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The modified Chaplygin gas (MCG) as an interacting model of holographic dark energy in which dark energy and dark matter are coupled together is investigated in this paper. Concretely, by studying the evolutions of related cosmological quantities such as density parameter Ω, equation of state w, deceleration parameter q and transition redshift z T , we find the evolution of the universe is from deceleration to acceleration, their present values are consistent with the latest observations, and the equation of state of holographic dark energy can cross the phantom divide w = −1. Furthermore, we put emphasis upon the geometrical diagnostics for our model, i.e., the statefinder and Om diagnostics. By illustrating the evolutionary trajectories in r − s, r − q, w -w and Om planes, we find that the holographic constant c and the coupling constant b play very important roles in the holographic dark energy (HDE) model. In addition, we also plot the LCDM horizontal lines in Om diagrams, and show the discrimination between the HDE and LCDM models. modified Chaplygin gas, interacting holographic dark energy, geometrical diagnostics PACS: 98.80.Es, 98.80.JkIt has been believed that the universe is undergoing a phase of accelerated expansion, which is indicated by such astronomical observations as Type Ia supernovae (SNe) [1], cosmic microwave background (CMB) anisotropy [2] and large scale structure (LSS) [3]. This implies that there is a mysterious component in the universe, which has a large negative pressure called dark energy (DE). The Wilkinson Microwave Anisotropy Probe (WMAP) satellite experiment indicates that the universe is spatially flat on a large scale, and the dark energy, dark matter (DM) and baryon matter in the universe make up about 73%, 23%, and 4%, respectively. Recently, there are some studies showing that the equation of state (EoS) of dark energy w X = p X ρ X might evolve from w X > −1 to w X < −1. When these SNe results are combined with WMAP 5-year data the 95% confidence limits on an unevolving EoS are −1.11 < w 0X < −0.86 [4]. More and more scenarios have been proposed as the candidates of DE to explain the accelerated expansion. What fits best with the observational data is the cosmological constant λ [5], which has the EoS w = −1, and is called the LCDM model in which *Corresponding author (email: ybwu61@163.com) the cosmological constant is combined with the cold dark matter. However, it is plagued with some problems, i.e., the "cosmic coincidence" problem [6] and the "fine tuning" problem [7]. A number of scalar field models have been constructed, such as quintessence [8], phantom [9], K-essence [10], quintom [11] and tachyon [12]. Furthermore, models such as Chaplygin gas (CG) [13] and modified Chaplygin gas (MCG) [14][15][16], which attempt to unify DE and DM, are proposed by allowing for a fluid with an EoS which evolves between the both.In recent years, the model has been stimulated by the holographic principle, i.e., the so-called holographic dark energy (HDE) has been put forward by Li...

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Constraints on holographic dark energy from the latest supernovae, galaxy clustering, and cosmic microwave background anisotropy observations

Cited by 204 publications

References 86 publications

Entropy in the Present and Early Universe: New Small Parameters and Dark Energy Problem

Entropy in the Present and Early Universe: New Small Parameters and Dark Energy Problem

Reexploration of interacting holographic dark energy model: cases of interaction term excluding the Hubble parameter

Modified Chaplygin gas as an interacting holographic dark energy model

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