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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Non-minimally coupled quintessence with sign-switching interaction
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abstract
We propose a new non-minimally coupled quintessence model to account for the late-time dark energy dynamics indicated by recent DESI measurements. Within this framework, the quintessence density begins to decrease only when it starts to dominate the universe, which naturally accounts for the late-time onset of dark energy weakening. The coupling also induces a sign change in the effective energy transfer between dark matter and dark energy during cosmic evolution. While the scalar field itself remains canonical and never crosses the phantom divide, the modified evolution of the dark matter density gives rise to an effective crossing behavior in the observationally inferred dark energy sector. Compared with both $\Lambda$CDM and $w_0w_a$CDM models, our model is favored more strongly by current cosmological data. This work may provide a promising avenue for understanding the observational late-time weakening of dark energy and the origin of its dynamics.
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astro-ph.CO 12years
2026 12representative citing papers
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.
Coupled SUGRA quintessence is preferred by current data at >4σ over the uncoupled case, with sign-changing interaction producing phantom-crossing behavior statistically similar to the CPL parametrization.
The ΛsCDM model with coupled dark sectors reduces the Hubble tension to 1.2σ via late-time expansion changes while keeping the early-universe sound horizon nearly unchanged.
Tensions in the supernova intercept a_B at z~0.01 in PantheonPlus and z~0.1 in DES-Y5 point to data systematics or inter-survey inconsistencies rather than new physics, aligning H0 measurements and reducing support for dynamical dark energy.
In the CQ-EXP model, fixed neutrino mass yields >3σ preference for β<0 and phantom crossing; freeing ∑mν,eff erases the distinction from w0waCDM.
Coupled quintessence-dark matter models can produce an apparent phantom-crossing effective equation of state matching DESI preferences if the scalar field begins frozen in the radiation era.
DESI data hint that dark energy evolves (w0>−1, wa<0, phantom crossing) at 2.5–4.2σ, but the same expansion history can also be produced by interacting dark sectors, modified gravity, or non-cold dark matter.
Effective phantom dark energy is a background-level reconstruction that does not imply fundamental pathologies such as ghost instabilities or null energy condition violation by the underlying stress tensor.
Global Bayesian evidence shows no statistically significant support for dynamical dark energy or phantom crossing despite limited local fit improvements in the w0wa parametrization.
citing papers explorer
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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.
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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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Coupled quintessence with a potential from supergravity exhibits sign-changing interaction
Coupled SUGRA quintessence is preferred by current data at >4σ over the uncoupled case, with sign-changing interaction producing phantom-crossing behavior statistically similar to the CPL parametrization.
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Alleviating the Hubble Tension Using $\Lambda$sCDM Model: A Coupled Dark Energy - Dark Matter Interaction
The ΛsCDM model with coupled dark sectors reduces the Hubble tension to 1.2σ via late-time expansion changes while keeping the early-universe sound horizon nearly unchanged.
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Cosmological intercept tension
Tensions in the supernova intercept a_B at z~0.01 in PantheonPlus and z~0.1 in DES-Y5 point to data systematics or inter-survey inconsistencies rather than new physics, aligning H0 measurements and reducing support for dynamical dark energy.
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Phantom-Divide Crossing in Exponentially Coupled Quintessence and the Role of Neutrino-Mass Freedom
In the CQ-EXP model, fixed neutrino mass yields >3σ preference for β<0 and phantom crossing; freeing ∑mν,eff erases the distinction from w0waCDM.
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Coupled Dark Energy and Dark Matter for DESI: An Effective Guide to the Phantom Divide
Coupled quintessence-dark matter models can produce an apparent phantom-crossing effective equation of state matching DESI preferences if the scalar field begins frozen in the radiation era.
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Dark Energy in the DESI Era: A Brief Review of Evidence, Beyond-$\Lambda$CDM Interpretations, and Tensions
DESI data hint that dark energy evolves (w0>−1, wa<0, phantom crossing) at 2.5–4.2σ, but the same expansion history can also be produced by interacting dark sectors, modified gravity, or non-cold dark matter.
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Effective Phantom Dark Energy: What Cosmological Reconstruction Does and Does Not Imply
Effective phantom dark energy is a background-level reconstruction that does not imply fundamental pathologies such as ghost instabilities or null energy condition violation by the underlying stress tensor.
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No evidence for phantom crossing: local goodness-of-fit improvements do not persist under global Bayesian model comparison
Global Bayesian evidence shows no statistically significant support for dynamical dark energy or phantom crossing despite limited local fit improvements in the w0wa parametrization.
- Constraints on Coupled Dark Energy in the DESI Era