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• W2790543291 abstract "We perform a comprehensive analysis of the most common early- and late-Universe solutions to the $H_0$, Ly-$alpha$, and $S_8$ discrepancies. When considered on their own, massive neutrinos provide a natural solution to the $S_8$ discrepancy at the expense of increasing the $H_0$ tension. If all extensions are considered simultaneously, the best-fit solution has a neutrino mass sum of $sim 0.4$ eV, a dark energy equation of state close to that of a cosmological constant, and no additional relativistic degrees of freedom. However, the $H_0$ tension, while weakened, remains unresolved. Motivated by this result, we perform a non-parametric reconstruction of the evolution of the dark energy fluid density (allowing for negative energy densities), together with massive neutrinos. When all datasets are included, there exists a residual $sim1.9sigma$ tension with $H_0$. If this residual tension remains in the future, it will indicate that it is not possible to solve the $H_0$ tension solely with a modification of the late-Universe dynamics within standard general relativity. However, we do find that it is possible to resolve the tension if either galaxy BAO or JLA supernovae data are omitted. We find that textit{negative} dark energy densities are favored near redshift $zsim2.35$ when including the Ly-$alpha$ BAO measurement (at $sim 2sigma$). This behavior may point to a negative curvature, but it is most likely indicative of systematics or at least an underestimated covariance matrix. Quite remarkably, we find that in the extended cosmologies considered in this work, the neutrino mass sum is always close to $0.4$ eV regardless of the choice of external datasets, as long as the $H_0$ tension is solved or significantly decreased." @default.
• W2790543291 created "2018-03-29" @default.
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• W2790543291 date "2018-06-06" @default.
• W2790543291 modified "2023-10-18" @default.
• W2790543291 title "Implications of an extended dark energy cosmology with massive neutrinos for cosmological tensions" @default.
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• W2790543291 doi "https://doi.org/10.1103/physrevd.97.123504" @default.
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