For PEDE and GOHDE models, the apparent high Hubble constant comes from dataset choice and priors; easing the tension requires a future violation of the null energy condition.
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What solves the Hubble tension in phenomenological dark energy models at background level?
For PEDE and GOHDE models, the apparent high Hubble constant comes from dataset choice and priors; easing the tension requires a future violation of the null energy condition.