Non-parametric reconstruction of non-minimally coupled gravity with a smoothness prior on CMB, DESI BAO, supernovae, and DES data yields a 2.8σ hint for coupling and a preference for phantom divide crossing stabilized by the coupling.
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Weakly dissipative quintessence explains DESI phantom crossing in dark energy without pathological dynamics.
Modified gravity below O(10) Mpc in a CPL dynamical dark energy background is required to suppress structure growth at low redshifts while satisfying CMB constraints from ISW and lensing.
Early dark energy resolves CMB-BAO tension and, combined with thawing quintessence, reduces overall cosmological tensions without phantom crossing.
The w†VCDM model shows a statistically significant preference for late-time quintessence-phantom crossing dark energy, raises the Hubble constant, and satisfies neutrino mass and Neff constraints from current cosmological datasets.
The QDEE model fits combined cosmological datasets better than Lambda CDM, shifts the Hubble constant higher, and shows strong Bayesian evidence in its favor.
Two three-parameter extensions of the mAH dark energy parametrization are compared to LambdaCDM, wCDM, CPL and others using CMB, DESI BAO, H(z), RSD and three SNIa samples, yielding Delta chi-squared improvements of 6-38 and 2-5 sigma tensions with LambdaCDM.
Bulk viscous fluid models for dark energy yield improved fits to supernova, BAO, and CMB data over LambdaCDM, especially in the interacting non-minimal case.
Horndeski gravity with shift symmetry and linear potential permits three mechanisms for crossing the phantom divide but none fit current data well without a cosmological constant.
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Late-time reconstruction of non-minimally coupled gravity with a smoothness prior
Non-parametric reconstruction of non-minimally coupled gravity with a smoothness prior on CMB, DESI BAO, supernovae, and DES data yields a 2.8σ hint for coupling and a preference for phantom divide crossing stabilized by the coupling.