Full DES data from SN+BAO+3x2pt yields w0=-0.84, wa=-0.44 with 2.2σ deviation from ΛCDM; adding DESI+CMB reaches 3.0σ while 3x2pt improves figure of merit by ~10%.
Tsujikawa, Crossing the phantom divide in scalar- tensor and vector-tensor theories, Phys
9 Pith papers cite this work, alongside 1 external citations. Polarity classification is still indexing.
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Asymptotic Cubic Galileon models can fit Planck+DESI+DES expansion history with phantom crossing and are tightly constrained by galaxy-ISW and void-force observables.
Under standard recombination, phantom-crossing dynamical dark energy is preferred at ~97–98.5% probability; early-time fixes to the Hubble tension erase that preference while creating severe ω_m tension with CMB.
Weakly dissipative quintessence explains DESI phantom crossing in dark energy without pathological dynamics.
Using Planck, DESI, supernovae, and redshift-space distortions, the authors infer that modified gravity, if present, must act only below ~30 Mpc and cannot modify the large scales previously considered.
Early dark energy resolves CMB-BAO tension and, combined with thawing quintessence, reduces overall cosmological tensions without phantom crossing.
Cosmological data can constrain only a handful of EFT parameters for single-scalar dark energy; extended models show modest preference over Λ but remain underdetermined and challenged by fifth forces and screening.
A two-field quintom model reproduces w0waCDM perturbation features and is mildly favored over it in Bayesian fits to BAO, CMB, and SNIa data.
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.
citing papers explorer
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Constraints on Dynamical Dark Energy from Multiple Probes in the Full Dark Energy Survey
Full DES data from SN+BAO+3x2pt yields w0=-0.84, wa=-0.44 with 2.2σ deviation from ΛCDM; adding DESI+CMB reaches 3.0σ while 3x2pt improves figure of merit by ~10%.
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Constraints on Horndeski Gravity with Phantom Crossing
Asymptotic Cubic Galileon models can fit Planck+DESI+DES expansion history with phantom crossing and are tightly constrained by galaxy-ISW and void-force observables.
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Exploring the interplay of late-time dynamical dark energy and new physics before recombination
Under standard recombination, phantom-crossing dynamical dark energy is preferred at ~97–98.5% probability; early-time fixes to the Hubble tension erase that preference while creating severe ω_m tension with CMB.
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Dissipative Dark Energy can explain the DESI phantom crossing
Weakly dissipative quintessence explains DESI phantom crossing in dark energy without pathological dynamics.
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Signatures of Modified Gravity on Linear Scales in a Dynamical Dark Energy Background
Using Planck, DESI, supernovae, and redshift-space distortions, the authors infer that modified gravity, if present, must act only below ~30 Mpc and cannot modify the large scales previously considered.
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Disentangling cosmic distance tensions with early and late dark energy
Early dark energy resolves CMB-BAO tension and, combined with thawing quintessence, reduces overall cosmological tensions without phantom crossing.
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The Status of Single Scalar Field Dark Energy
Cosmological data can constrain only a handful of EFT parameters for single-scalar dark energy; extended models show modest preference over Λ but remain underdetermined and challenged by fifth forces and screening.
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Quintom Model Perturbations
A two-field quintom model reproduces w0waCDM perturbation features and is mildly favored over it in Bayesian fits to BAO, CMB, and SNIa data.
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Charging Across the Phantom Divide with Modified Gravity
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.