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Quintessential interpretation of the evolving dark energy in light of DESI
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abstract
The recent result of Dark Energy Spectroscopic Instrument (DESI) in combination with other cosmological data shows evidence of the evolving dark energy parameterized by $w_0w_a$CDM model. We interpret this result in terms of a quintessential scalar field and demonstrate that it can explain the DESI result even though it becomes eventually phantom in the past. Relaxing the assumption on the functional form of the equation-of-state parameter $w=w(a)$, we also discuss a more realistic quintessential model. The implications of the DESI result for Swampland conjectures, cosmic birefringence, and the fate of the Universe are discussed as well.
Forward citations
Cited by 7 Pith papers
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General Relativistic Entropic Acceleration at the perturbation level: a CLASS implementation and first Boltzmann-code constraints
First full Boltzmann-code implementation of entropic dark energy, with MCMC constraints from CMB+BAO+SN, yields α≈1 and a fit statistically indistinguishable from ΛCDM.
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Do we really need alternatives to the $\omega_0\omega_a$CDM parameterization after the DESI DR2?
In a common physically motivated pivot basis, the standard CPL parameterization is mildly preferred over the fafbCDM density expansion and reproduces quintessence backgrounds at least as well.
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Robust Preference for Dark Sector Interactions
Interacting dark matter–dark energy models fit DESI BAO and CMB data as well as evolving-dark-energy (CPL) models, with a coupling preference that persists under DES-Dovekie supernova recalibration.
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Electroweak instantons alone do not produce Majoron domain walls; a tiny instanton mass from B+L breaking is cosmologically negligible and can act as a bias or dark energy.
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The Lifespan of our Universe
If the axion dark energy model with a negative cosmological constant is the true explanation of DES/DESI data, the universe will end in a big crunch at a total age of about 33 billion years.
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An overview of what current data can (and cannot yet) say about evolving dark energy
The apparent preference for evolving dark energy depends strongly on which supernova catalog and which BAO survey are used, and is not robust across all independent data combinations.
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A short review on Quintom dark energy theory
Quintom dark energy models permit the equation of state to cross w=-1, supporting bouncing cosmologies and CMB-based tests of dark energy nature.
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