Modified gravity below O(10) Mpc in a CPL dynamical dark energy background is required to suppress structure growth at low redshifts while satisfying CMB constraints from ISW and lensing.
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An interacting dark sector model with Yukawa-coupled fermionic DM and Born-Infeld tachyonic scalar produces recent double phantom crossing in effective w_DE, fits DESI+Planck+SN data, and predicts ultralight DM mass of order 1.9e-3 eV under naturalness assumptions.
Planck PR4 CMB data mildly favors dynamical dark energy, but this preference weakens when accounting for possible excess smoothing, indicating the signal may partly arise from data processing issues.
Evidence for dynamical dark energy in the w0waCDM framework is strongly dataset-dependent, driven by mismatches in low-redshift BAO distance ratios that produce divergent expansion histories and inconsistent Hubble tension relief.
The w†VCDM model shows a statistically significant preference for late-time quintessence-phantom crossing dark energy, raises the Hubble constant, and satisfies neutrino mass and Neff constraints from current cosmological datasets.
The QDEE model fits combined cosmological datasets better than Lambda CDM, shifts the Hubble constant higher, and shows strong Bayesian evidence in its favor.
DESI-DR2 angular diameter distances and SNeIa luminosity distances are statistically consistent with the Etherington relation, yielding a constraint on SNeIa absolute magnitude evolution of dM/dz = 0.07 ± 0.07.
Quintessence models with standard potentials give only modest improvements over Lambda to DESI data on evolving dark energy, while non-minimal couplings allow temporary phantom behavior but face tight gravity constraints except for carefully selected narrow ranges.
citing papers explorer
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Signatures of Modified Gravity Below $\mathcal{O}(10)$ Mpc in a Dynamical Dark Energy Background
Modified gravity below O(10) Mpc in a CPL dynamical dark energy background is required to suppress structure growth at low redshifts while satisfying CMB constraints from ISW and lensing.
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Interacting Dark Sector field theory with phantom crossing
An interacting dark sector model with Yukawa-coupled fermionic DM and Born-Infeld tachyonic scalar produces recent double phantom crossing in effective w_DE, fits DESI+Planck+SN data, and predicts ultralight DM mass of order 1.9e-3 eV under naturalness assumptions.
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Is the $w_0w_a$CDM cosmological parameterization evidence for dark energy dynamics partially caused by the excess smoothing of Planck PR4 CMB anisotropy data?
Planck PR4 CMB data mildly favors dynamical dark energy, but this preference weakens when accounting for possible excess smoothing, indicating the signal may partly arise from data processing issues.
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Probing Dynamical Dark Energy with Late-Time Data: Evidence, Tensions, and the Limits of the $w_0w_a$CDM Framework
Evidence for dynamical dark energy in the w0waCDM framework is strongly dataset-dependent, driven by mismatches in low-redshift BAO distance ratios that produce divergent expansion histories and inconsistent Hubble tension relief.
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Joint Constraints on Neutrinos and Dynamical Dark Energy in Minimally Modified Gravity
The w†VCDM model shows a statistically significant preference for late-time quintessence-phantom crossing dark energy, raises the Hubble constant, and satisfies neutrino mass and Neff constraints from current cosmological datasets.
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Probing late-time deviations from $\Lambda$CDM with a quadratic dark energy expansion
The QDEE model fits combined cosmological datasets better than Lambda CDM, shifts the Hubble constant higher, and shows strong Bayesian evidence in its favor.
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Cosmology-Independent Constraints on the Etherington Relation and SNeIa Absolute Magnitude Evolution from DESI-DR2
DESI-DR2 angular diameter distances and SNeIa luminosity distances are statistically consistent with the Etherington relation, yielding a constraint on SNeIa absolute magnitude evolution of dM/dz = 0.07 ± 0.07.
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Comparing Minimal and Non-Minimal Quintessence Models to 2025 DESI Data
Quintessence models with standard potentials give only modest improvements over Lambda to DESI data on evolving dark energy, while non-minimal couplings allow temporary phantom behavior but face tight gravity constraints except for carefully selected narrow ranges.
- Exploring the interplay of late-time dynamical dark energy and new physics before recombination