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2021-$H_0$ Odyssey: Closed, Phantom and Interacting Dark Energy Cosmologies
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abstract
Up-to-date cosmological data analyses have shown that \textit{(a)} a closed universe is preferred by the Planck data at more than $99\%$ CL, and \textit{(b)} interacting scenarios offer a very compelling solution to the Hubble constant tension. In light of these two recent appealing scenarios, we consider here an interacting dark matter-dark energy model with a non-zero spatial curvature component and a freely varying dark energy equation of state in both the quintessential and phantom regimes. When considering Cosmic Microwave Background data only, a phantom and closed universe can perfectly alleviate the Hubble tension, without the necessity of a coupling among the dark sectors. Accounting for other possible cosmological observations compromises the viability of this very attractive scenario as a global solution to current cosmological tensions, either by spoiling its effectiveness concerning the $H_0$ problem, as in the case of Supernovae Ia data, or by introducing a strong disagreement in the preferred value of the spatial curvature, as in the case of Baryon Acoustic Oscillations.
Forward citations
Cited by 6 Pith papers
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BAO miscalibration cannot rescue late-time solutions to the Hubble tension
Even after rescaling BAO data to prefer H0≈73 km/s/Mpc, none of six tested late-time dark-energy models can resolve the Hubble tension once unanchored SNeIa and CMB geometry are included.
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Quasar cosmology II: joint analyses with Cosmic Microwave Background
Quasar, supernova, BAO, DES, and CMB data are jointly compatible only in an interacting dark-energy model, not in Lambda-CDM, wCDM, or CPL.
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Background-level reconstruction of scalar-field potentials from dark-energy histories and comparison with analytic potential families
A background reconstruction maps prescribed ρ_de(z) histories to V(φ) and ranks analytic potentials by Bayesian evidence, with exponential preferred for CPL and shifted-tanh for sign-switching targets.
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Controlled Tension Forecasting: Quantifying Cross-Probe Biases in $\omega_0\omega_a$CDM
Controlled mock analyses show that cross-probe calibration tensions — in matter density, H0, supernova brightness, or sound horizon — can fake 3–10σ apparent dynamical-dark-energy signals while the true cosmology is ΛCDM.
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Is Dark Energy an Effective Manifestation of Non-equilibrium Thermodynamics? -- Insights from DESI
Two phenomenological dark matter creation rates can reproduce the accelerated expansion of the universe and fit current background data as well as or slightly better than LambdaCDM for some DESI-based data combinations.
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Solving an Interacting Quintessence Model with a Sound Horizon Initial Condition and its Observational Constraints
An interacting quintessence model with initial conditions set by the CMB sound horizon angle increases H0 with coupling strength, but observational constraints show it does not resolve the H0 or S8 tensions.
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