Cosmological Perturbations and the Running Cosmological Constant Model

Velasquez-Toribio, A. M.

doi:10.1142/s0218271812500265

Cited by 14 publications

(11 citation statements)

References 109 publications

(112 reference statements)

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“…For example, in Refs. [53][54][55][56], the cosmological constant is rewritten as Λ = Λ(H) with H = ∇ µ U µ /3. In this work, we follow the perturbation method in Refs.…”

Section: Introductionmentioning

confidence: 99%

Observational constraints on running vacuum model

Zhang¹,

Lee²,

Geng³

2019

Chinese Phys. C

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We investigate the power spectra of the CMB temperature and matter density in the running vacuum model (RVM) with the time-dependent cosmological constant of Λ = 3νH 2 + Λ 0 , where H is the Hubble parameter. In this model, dark energy decreases in time and decays to both matter and radiation. By using the Markov chain Monte Carlo method, we constrain the model parameter ν as well as the cosmological observables. Explicitly, we obtain ν ≤ 1.54 × 10 −4 (68% confidence level) in the RVM with the best-fit χ 2 RVM = 13968.8, which is slightly smaller than χ 2 ΛCDM = 13969.8 in the ΛCDM model of ν = 0. * Electronic address:

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“…For example, in Refs. [53][54][55][56], the cosmological constant is rewritten as Λ = Λ(H) with H = ∇ µ U µ /3. In this work, we follow the perturbation method in Refs.…”

Section: Introductionmentioning

confidence: 99%

Observational constraints on running vacuum model

Zhang¹,

Lee²,

Geng³

2019

Chinese Phys. C

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“…For example, vacuum fluctuations of free fields can support an averaged density proportional to the fourth-power of the Hubble expansion, V ∝ H 4 [12]. Such a vacuum energy would not in itself support an accelerated expansion, but other forms such as V ∝ H have been proposed [13] better able to match the observational data [14][15][16][17][18]. It is not clear whether or how such time-dependent vacuum models can be compared with observations in an inhomogeneous universe.…”

Section: Introductionmentioning

confidence: 99%

Inhomogeneous vacuum energy

Wands

De-Santiago

Wang

2012

Class. Quantum Grav.

133

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Vacuum energy remains the simplest model of dark energy which could drive the accelerated expansion of the Universe without necessarily introducing any new degrees of freedom. Inhomogeneous vacuum energy is necessarily interacting in general relativity. Although the four-velocity of vacuum energy is undefined, an interacting vacuum has an energy transfer and the vacuum energy defines a particular foliation of spacetime with spatially homogeneous vacuum energy in cosmological solutions. It is possible to give a consistent description of vacuum dynamics and in particular the relativistic equations of motion for inhomogeneous perturbations given a covariant prescription for the vacuum energy, or equivalently the energy transfer four-vector, and we construct gauge-invariant vacuum perturbations. We show that any dark energy cosmology can be decomposed into an interacting vacuum+matter cosmology whose inhomogeneous perturbations obey simple first-order equations.

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“…For this end, we follow Ref. [32] and assume the transfer function BBKS [59,60], given by the expression T (z) = ln (1 + 2.34q) 2.34q 1 + 3.89q + 16.1q 2 + 5.64q 3 + 6.71q 4 −1/4 ,…”

Section: Power Spectrummentioning

confidence: 99%

Constraints from observational data for a running cosmological constant and warm dark matter with curvature

Ruiz,

Fabris,

Velasquez-Toribio

et al. 2020

Preprint

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It is known than the inclusion of spatial curvature can modify the evolution of matter perturbations, and affect the Large Scale Structure (LSS) formation. We quantify the effects of the non-zero space curvature in terms of LSS formation for a cosmological model with a running vacuum energy density and a warm dark matter component. The evolution of density perturbations and the modified shape of its power spectrum are constructed and analyzed.

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Cosmological Perturbations and the Running Cosmological Constant Model

Cited by 14 publications

References 109 publications

Observational constraints on running vacuum model

Observational constraints on running vacuum model

Inhomogeneous vacuum energy

Constraints from observational data for a running cosmological constant and warm dark matter with curvature

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