Constraints on the sum of the neutrino masses in dynamical dark energy models with 
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 are tighter than those obtained in 
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Vagnozzi, Sunny; Dhawan, Suhail; Gerbino, Martina; Freese, Katherine; Goobar, A.; Mena, Olga

doi:10.1103/physrevd.98.083501

Cited by 195 publications

(125 citation statements)

References 232 publications

(231 reference statements)

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“…We find, in general, that the constraints on the dark radiation sector physics are quite close to those found within the minimal ΛCDM cosmology. The derived bounds are almost independent of the dark energy regime (phantom versus quintessence), contrary to the case without a dark coupling [71,72]. We find a total neutrino mass M ν < 0.15 eV and a number of effective relativistic degrees of freedom of N eff = 3.03 +0.…”

Section: Discussionmentioning

confidence: 60%

All-inclusive interacting dark sector cosmologies

et al. 2020

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In this paper we explore possible extensions of Interacting Dark Energy cosmologies, where Dark Energy and Dark Matter interact non-gravitationally with one another. In particular, we focus on the neutrino sector, analyzing the effect of both neutrino masses and the effective number of neutrino species. We consider the Planck 2018 legacy release data combined with several other cosmological probes, finding no evidence for new physics in the dark radiation sector. The current neutrino constraints from cosmology should be therefore regarded as robust, as they are not strongly dependent on the dark sector physics, once all the available observations are combined. Namely, we find a total neutrino mass Mν < 0.15 eV and a number of effective relativistic degrees of freedom of N eff = 3.03 +0.33 −0.33 , both at 95% CL, which are close to those obtained within the ΛCDM cosmology, Mν < 0.12 eV and N eff = 3.00 +0.36 −0.35 for the same data combination. PACS numbers: 98.80.-k, 95.35.+d, 95.36.+x, 98.80.Es.

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Section: Discussionmentioning

confidence: 60%

All-inclusive interacting dark sector cosmologies

et al. 2020

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“…These have focused on the DE equation of state (EoS) w x and its time evolution, or on models of modified gravity that can account for DE, by studying imprints on the background evolution and on the late-time growth of structure (see e.g. Ishak et al 2006;Mena et al 2006;De Felice et al 2008;Giannantonio et al 2010;Lombriser et al 2012;Martinelli et al 2012;Hu et al 2016;Nunes et al 2017a,b;Renk et al 2017;Peirone et al 2018;Vagnozzi et al 2018;Du et al 2019;Yang et al 2019a), and finally on the propagation of astrophysical gravitational waves (see e.g. Creminelli & Vernizzi 2017;Sakstein & Jain 2017;Ezquiaga & Zumalacárregui 2017;Boran et al 2018;Baker et al 2017;Visinelli et al 2018;Crisostomi & Koyama 2018;Langlois et al 2018;Ezquiaga & Zumalacárregui 2018;.…”

Section: Introductionmentioning

confidence: 99%

Do we have any hope of detecting scattering between dark energy and baryons through cosmology?

Vagnozzi

Visinelli

Mena

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We consider the possibility that dark energy and baryons might scatter off each other. The type of interaction we consider leads to a pure momentum exchange, and does not affect the background evolution of the expansion history. We parametrize this interaction in an effective way at the level of Boltzmann equations. We compute the effect of dark energy-baryon scattering on cosmological observables, focusing on the Cosmic Microwave Background (CMB) temperature anisotropy power spectrum and the matter power spectrum. Surprisingly, we find that even huge dark energy-baryon cross-sections σ xb ∼ O(b), which are generically excluded by non-cosmological probes such as collider searches or precision gravity tests, only leave an insignificant imprint on the observables considered. In the case of the CMB temperature power spectrum, the only imprint consists in a sub-percent enhancement or depletion of power (depending whether or not the dark energy equation of state lies above or below −1) at very low multipoles, which is thus swamped by cosmic variance. These effects are explained in terms of differences in how gravitational potentials decay in the presence of a dark energy-baryon scattering, which ultimately lead to an increase or decrease in the latetime integrated Sachs-Wolfe power. Even smaller related effects are imprinted on the matter power spectrum. The imprints on the CMB are not expected to be degenerate with the effects due to altering the dark energy sound speed. We conclude that, while strongly appealing, the prospects for a direct detection of dark energy through cosmology do not seem feasible when considering realistic dark energy-baryon cross-sections. As a caveat, our results hold to linear order in perturbation theory.

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“…On the other hand, the neutrinos properties play a crucial role in the dynamics of our Universe, by inferring direct changes in the important cosmological sources, and consequently, in the determination of cosmological parameters (see an incomplete list of recent and past works [62,63,64,65,66,67,68,69,70,71,72,73,74,75,76] and references therein). The standard parameters that characterize these effects are the effective number of neutrino species N eff and the total neutrino mass scale M ν .…”

Section: Introductionmentioning

confidence: 99%

Dark calling dark: interaction in the dark sector in presence of neutrino properties after Planck CMB final release

Yang¹,

Pan²,

Nunes³

et al. 2020

J. Cosmol. Astropart. Phys.

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We investigate a well known scenario of interaction in the dark sector, where the vacuum energy is interacting with cold dark matter throughout the cosmic evolution in light of the cosmic microwave background (CMB) data from final Planck 2018 release. In addition to this minimal scenario, we generalize the model baseline by including the properties of neutrinos, such as the neutrino mass scale (Mν ) and the effective number of neutrino species (N eff ) as free parameters, in order to verify the possible effects that such parameters might generate on the coupling parameter, and vice versa. As already known, we confirm that in light of Planck 2018 data, such dark coupling can successfully solve the H0 tension (with and without the presence of neutrinos). Concerning the properties of neutrinos, we find that Mν may be wider than expected within the ΛCDM model and N eff is fully compatible with three neutrino species (similar to ΛCDM prevision). The parameters characterizing the properties of neutrinos do not correlate with the coupling parameter of the interaction model. When considering the joint analysis of CMB from Planck 2018 and an estimate of H0 from Hubble Space Telescope 2019 data, we find an evidence for a non-null value of the coupling parameter at more than 3σ confidence-level. We discuss also the inclusion the baryon acoustic oscillations data in combination with Planck 2018 and implications for the scenarios addressed. Our main results updating the dark sectors' interaction and neutrino properties in the model baseline, represent a new perspective in this direction. Clearly, a possible new physics in light of some dark interaction between dark energy and dark matter can serve as an alternative to ΛCDM scenario to explain the observable Universe, mainly in light of the current tension on H0.

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Constraints on the sum of the neutrino masses in dynamical dark energy models with w(z)≥−1 are tighter than those obtained in Λ

Cited by 195 publications

References 232 publications

All-inclusive interacting dark sector cosmologies

All-inclusive interacting dark sector cosmologies

Do we have any hope of detecting scattering between dark energy and baryons through cosmology?

Dark calling dark: interaction in the dark sector in presence of neutrino properties after Planck CMB final release

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