Model-independent reconstruction shows that early-universe modifications resolving the Hubble tension exist at the background level, requiring a smooth ~15% pre-recombination expansion rate enhancement.
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Model-independent reconstruction finds 96.7-98.5% probability of phantom crossing if recombination is standard, but early new physics to ease Hubble tension weakens this preference while requiring unrealistically high matter density.
A 0.19 mag step in supernova absolute magnitude at 20 Mpc improves data fit and increases the Hubble constant by 2% while leaving matter density and dark energy parameters stable.
New cosmological data mildly favor a small coupling between dark matter and a scalar dark energy field at |β| ≈ 0.03 while allowing an effective phantom-crossing equation of state.
citing papers explorer
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Geometric Constraints on the Pre-Recombination Expansion History from the Hubble Tension
Model-independent reconstruction shows that early-universe modifications resolving the Hubble tension exist at the background level, requiring a smooth ~15% pre-recombination expansion rate enhancement.
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Exploring the interplay of late-time dynamical dark energy and new physics before recombination
Model-independent reconstruction finds 96.7-98.5% probability of phantom crossing if recombination is standard, but early new physics to ease Hubble tension weakens this preference while requiring unrealistically high matter density.
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Impact of the SNe Ia Magnitude Transition at 20 Mpc on Cosmological Parameter Estimation
A 0.19 mag step in supernova absolute magnitude at 20 Mpc improves data fit and increases the Hubble constant by 2% while leaving matter density and dark energy parameters stable.
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Constraints on Coupled Dark Energy in the DESI Era
New cosmological data mildly favor a small coupling between dark matter and a scalar dark energy field at |β| ≈ 0.03 while allowing an effective phantom-crossing equation of state.