The Hubble constant tension: current status and future perspectives through new cosmological probes

Dainotti, Maria Giovanna; De Simone, Biagio; Montani;, Giovanni; Schiavone;, Tiziano; Lambiase., Gaetano

doi:10.22323/1.436.0235

Cited by 10 publications

(5 citation statements)

References 251 publications

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“…Assuming that ( 57)-( 59) can be used to constrain the cosmological evolution of G, let us tentatively use these limits (in order of magnitude) in combination with Equation (56) to constrain the parameter ν eff . The last equation implies φ −3ν eff H 0 for H H 0 1.023h × 10 −10 yr −1 around our time (h 0.7) The previous relation is equivalent to Ġ/G 3ν eff H 0 to order ν eff .…”

Section: Background Equationsmentioning

confidence: 99%

“…Specific realizations of the noticed double condition for the DE fluid can be found in the literature, e.g., in the context of the ΛXCDM model [53,54], closely related to the idea of the running vacuum to be discussed in the present work, see below. For detailed reviews on these tensions and other challenges afflicting the concordance ΛCDM model; see, e.g., [33,55,56] and the long list of references quoted therein bearing relation to these matters.…”

Section: Introductionmentioning

confidence: 99%

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Running Vacuum in the Universe: Phenomenological Status in Light of the Latest Observations, and Its Impact on the σ8 and H0 Tensions

et al. 2023

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A substantial body of phenomenological and theoretical work over the last few years strengthens the possibility that the vacuum energy density (VED) of the universe is dynamical, and in particular that it adopts the ‘running vacuum model’ (RVM) form, in which the VED evolves mildly as δρvac(H)∼νeffmPl2OH2, where H is the Hubble rate and νeff is a (small) free parameter. This dynamical scenario is grounded on recent studies of quantum field theory (QFT) in curved spacetime and also on string theory. It turns out that what we call the ‘cosmological constant’, Λ, is no longer a rigid parameter but the nearly sustained value of 8πG(H)ρvac(H) around any given epoch H(t), where G(H) is the gravitational coupling, which can also be very mildly running (logarithmically). Of particular interest is the possibility suggested in past works that such a running may help to cure the cosmological tensions afflicting the ΛCDM. In the current study, we reanalyze the RVM in full and we find it becomes further buttressed. Using modern cosmological data, namely a compilation of the latest SNIa+BAO+H(z)+LSS+CMB observations, we probe to what extent the RVM provides a quality fit better than the concordance ΛCDM model, with particular emphasis on its impact on the σ8 and H0 tensions. We utilize the Einstein–Boltzmann system solver CLASS and the Monte Carlo sampler MontePython for the statistical analysis, as well as the statistical DIC criterion to compare the running vacuum against the rigid vacuum (νeff=0). On fundamental grounds, νeff receives contributions from all the quantized matter fields in FLRW spacetime. We show that with a tiny amount of vacuum dynamics (νeff≪1) the global fit can improve significantly with respect to the ΛCDM and the mentioned tensions may subside to inconspicuous levels.

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Section: Background Equationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Running Vacuum in the Universe: Phenomenological Status in Light of the Latest Observations, and Its Impact on the σ8 and H0 Tensions

et al. 2023

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“…A large number of articles have been published with proposed solutions to the Hubble tension, but so far, no solution has been generally accepted. A review [4] with 709 references has recently been published by Maria Dainotti and co-workers.…”

Section: Introductionmentioning

confidence: 99%

Anisotropic Generalization of the ΛCDM Universe Model with Application to the Hubble Tension

Grøn

2024

Symmetry

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I deduce an exact and analytic Bianchi type I solution of Einstein’s field equations, which generalizes the isotropic ΛCDM universe model to a corresponding model with anisotropic expansion. The main point of the article is to present the anisotropic generalization of the ΛCDM universe model in a way suitable for investigating how anisotropic expansion modifies observable properties of the ΛCDM universe model. Although such generalizations of the isotropic ΛCDM universe model have been considered earlier, they have never been presented in this form before. Several physical properties of the model are pointed out and compared with properties of special cases, such as the isotropic ΛCDM universe model. The solution is then used to investigate the Hubble tension. It has recently been suggested that the cosmic large-scale anisotropy may solve the Hubble tension. I consider those earlier suggestions and find that the formulae of these papers lead to the result that the anisotropy of the cosmic expansion is too small to solve the Hubble tension. Then, I investigate the problem in a new way, using the exact solution of the field equations. This gives the result that the cosmic expansion anisotropy is still too small to solve the Hubble tension in the general Bianchi type I universe with dust and LIVE (Lorentz Invariant Vacuum Energy with a constant energy density, which is represented by the cosmological constant) and anisotropic expansion in all three directions—even if one neglects the constraints coming from the requirement that the anisotropy should be sufficiently small so that it does not have any significant effect upon the results coming from the calculations of the comic nucleosynthesis during the first ten minutes of the universe. If this constraint is taken into account, the cosmic expansion anisotropy is much too small to solve the Hubble tension.

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“…The cosmological constant has been added to the Einstein-Hilbert (EH) action to address some of the aforementioned cosmological issues. Nonetheless, this ΛCDM model has its own challenges, the most significant of which are the cosmological constant problem [11][12][13][14][15], Hubble tension problem [7,16,17], and fine-tuning and coincident problem [18,19].…”

Section: Introductionmentioning

confidence: 99%

Fractional Scalar Field Cosmology

Rasouli,

Cheraghchi,

Moniz

2024

Fractal Fract

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Considering the Friedmann–Lemaître–Robertson–Walker (FLRW) metric and the Einstein scalar field system as an underlying gravitational model to construct fractional cosmological models has interesting implications in both classical and quantum regimes. Regarding the former, we just review the most fundamental approach to establishing an extended cosmological model. We demonstrate that employing new methodologies allows us to obtain exact solutions. Despite the corresponding standard models, we cannot use any arbitrary scalar potentials; instead, it is determined from solving three independent fractional field equations. This article concludes with an overview of a fractional quantum/semi-classical model that provides an inflationary scenario.

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The Hubble constant tension: current status and future perspectives through new cosmological probes

Cited by 10 publications

References 251 publications

Running Vacuum in the Universe: Phenomenological Status in Light of the Latest Observations, and Its Impact on the σ8 and H0 Tensions

Running Vacuum in the Universe: Phenomenological Status in Light of the Latest Observations, and Its Impact on the σ8 and H0 Tensions

Anisotropic Generalization of the ΛCDM Universe Model with Application to the Hubble Tension

Fractional Scalar Field Cosmology

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