All-inclusive interacting dark sector cosmologies

Yang, Weiqiang; Valentino, Eleonora Di; Mena, Olga; Pan, Supriya; Nunes, Rafael C.

doi:10.1103/physrevd.101.083509

“…This result is very close to the result of [121], the case IDE+ m ν , using (CMB + Pantheon + CC data) with m ν < 0.255 eV at 95% CL. Both the model is similar to ours and the data used includes Pantheon data.…”

Section: Ide+ M νsupporting

confidence: 89%

Constraining neutrino mass in dark energy dark matter interaction and comparison with 2018 Planck results

Amiri

¹

,

Salehi

²

,

Noroozi

³

2021

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In this paper, we investigate the constraints on the total neutrino mass $$\sum m_{\nu }$$ ∑ m ν in a cosmological model in which dark energy and neutrinos are coupled such that the mass of the neutrinos and potentials are function of the scalar field as $$m_{\nu }=m_{0}\exp (\frac{\alpha \phi }{m_{pl}})$$ m ν = m 0 exp ( α ϕ m pl ) and $$V(\phi )=m_{pl}^{4}\exp (\frac{-\lambda \phi }{m_{pl}})$$ V ( ϕ ) = m pl 4 exp ( - λ ϕ m pl ) respectively. The observational data used in this work include the type Ia supernovae (SN) observation (Pantheon compilation), CC, CMB and BAO data. We find that the neutrino mass is tightly constrained to $$\sum m_{\nu }< 0.125$$ ∑ m ν < 0.125 eV 95% Confidence Level (C.L.) and the effective extra relativistic degrees of freedom to be $$N_{eff}=2.955^{+0.11}_{-0.12}$$ N eff = 2 . 955 - 0.12 + 0.11 68% C.L in agreement with the Standard Model prediction $$ N_{eff} = 3.046$$ N eff = 3.046 , matter-radiation equality, $$z_{eq}=3389^{+24}_{25}$$ z eq = 3389 25 + 24 (68% C.L). These results are in good agreement with the results of Planck 2018 where the limit of the total neutrino mass is $$\sum m_{\nu }<0.12$$ ∑ m ν < 0.12 eV (95% C.L., TT, TE, EE + lowE + lensing + BAO) , $$N_{eff}=2.99^{+0.17}_{-0.17}$$ N eff = 2 . 99 - 0.17 + 0.17 (68% C.L., TT, TE, EE + lowE + lensing + BAO) and $$z_{eq}=3387^{+21}_{21}$$ z eq = 3387 21 + 21 (68% C.L TT, TE, EE + lowE + lensing + BAO).

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“…For an interacting dark energy with a quintessencelike equation of state, the CDM energy density Ω c h 2 is always smaller than in a ΛCDM model: indeed, only an upper limit for this cosmological parameter is found [65,77,89]. The most interesting feature of this IDE1q scenario is that, even if the well-known anticorrelation between w x and H 0 is present, see Fig.…”

Section: Ide1qmentioning

confidence: 89%

“…For an interacting dark energy with a phantomlike equation of state, the cold dark matter (CDM) energy density Ω c h 2 is larger than in the ΛCDM model, provided the energy transfer is from the DE to the DM sector [65,77]. Furthermore, due to the strong degeneracy between w x and H 0 , see Fig.…”

Section: Ide1pmentioning

confidence: 98%

“…Following our pioneering previous work [55] we shall consider here a time-dependent coupling in nonminimal cosmologies. Given the fact that neutrinos can play a nonstandard role within nonminimal dark energy scenarios [56][57][58][59][60][61][62][63][64][65][66], we extend our previous analyses by inspecting the impact of neutrino properties within interacting cosmologies with a time-dependent coupling. We also generalize the work of Ref.…”

Section: Introductionmentioning

confidence: 99%

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Dynamical dark sectors and neutrino masses and abundances

Yang

¹

,

Valentino

²

,

Mena

³

et al. 2020

Self Cite

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We investigate generalized interacting dark matter-dark energy scenarios with a time-dependent coupling parameter, allowing also for freedom in the neutrino sector. The models are tested in the phantom and quintessence regimes, characterized by equations of state, w x < −1 and w x > −1, respectively. Our analyses show that for some of the scenarios, the existing tensions on the Hubble constant H 0 and on the clustering parameter S 8 can be significantly alleviated. The relief is either due to (a) a dark energy component which lies within the phantom region or (b) the presence of a dynamical coupling in quintessence scenarios. The inclusion of massive neutrinos into the interaction schemes does not affect either the constraints on the cosmological parameters or the bounds on the total number or relativistic degrees of freedom N eff , which are found to be extremely robust and, in general, strongly consistent with the canonical prediction N eff ¼ 3.045. The most stringent bound on the total neutrino mass M ν is M ν < 0.116 eV and it is obtained within a quintessence scenario in which the matter mass-energy density is only mildly affected by the presence of a dynamical dark sector coupling.

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“…There are many approaches in order to investigate the DE, e.g., the dynamical DE, phantom DE, quintessence, Chaplygin gas, holographic DE, the interaction between DE and DM, phenomenological emergent DE, and early DE (see Refs. [18,[20][21][22][23][24][25][26][27][28]). Among several models to investigate the DE, the thermodynamic approach has been widely investigated (see, e.g., Refs.…”

Section: Introductionmentioning

confidence: 99%

Growth of matter perturbations in the extended viscous dark energy models

Silva

¹

,

Silva

²

2021

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In this work, we study the extended viscous dark energy models in the context of matter perturbations. To do this, we assume an alternative interpretation of the flat Friedmann–Lemaître–Robertson–Walker Universe, through the nonadditive entropy and the viscous dark energy. We implement the relativistic equations to obtain the growth of matter fluctuations for a smooth version of dark energy. As result, we show that the matter density contrast evolves similarly to the $$\Lambda $$ Λ CDM model in high redshift; however, in late time, it is slightly different from the standard model. Using the latest geometrical and growth rate observational data, we carry out a Bayesian analysis to constrain parameters and compare models. We see that our viscous models are compatible with cosmological probes, and the $$\Lambda $$ Λ CDM recovered with a $$1\sigma $$ 1 σ confidence level. The viscous dark energy models relieve the tension of $$H_0$$ H 0 in $$2 \sim 3 \sigma $$ 2 ∼ 3 σ . Yet, by involving the $$\sigma _8$$ σ 8 tension, some models can alleviate it. In the model selection framework, the data discards the extended viscous dark energy models.

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All-inclusive interacting dark sector cosmologies

Cited by 62 publications

References 103 publications

Constraining neutrino mass in dark energy dark matter interaction and comparison with 2018 Planck results

Constraining neutrino mass in dark energy dark matter interaction and comparison with 2018 Planck results

Dynamical dark sectors and neutrino masses and abundances

Growth of matter perturbations in the extended viscous dark energy models

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