Two-field axion-like early dark energy reduces Hubble tension to 1.5 sigma residual and improves high-ell CMB fits over single-field models.
A larger value for $H_0$ by an evolving gravitational constant
6 Pith papers cite this work, alongside 120 external citations. Polarity classification is still indexing.
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abstract
We provide further evidence that a massless cosmological scalar field with a non-minimal coupling to the Ricci curvature of the type $M^2_{\rm pl}(1+\xi \sigma^n/M_{\rm pl}^n) $ alleviates the existing tension between local measurements of the Hubble constant and its inference from CMB anisotropies and baryonic acoustic oscillations data in presence of a cosmological constant. In these models, the expansion history is modified compared to $\Lambda$CDM at early time, mimicking a change in the effective number of relativistic species, and gravity weakens after matter-radiation equality. Compared to $\Lambda$CDM, a quadratic ($n=2$) coupling increases the Hubble constant when {\em Planck} 2018 (alone or in combination with BAO and SH0ES) measurements data are used in the analysis. Negative values of the coupling, for which the scalar field decreases, seem favored and consistency with Solar System can be naturally achieved for a large portion of the parameter space without the need of any screening mechanism. We show that our results are robust to the choice of $n$, also presenting the analysis for $n=4$.
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EDE models increase inferred α_s from CMB data, strengthening tension with USR PBH models that predict negative running.
A unified post-Newtonian analysis shows that metric vs Palatini scalar-tensor gravity can yield different γ, β and Yukawa suppression, with Palatini f(R̂) recovering GR’s exterior PN limit for point sources.
A swampland-inspired DM-EDE coupling is tested against DESI DR2 BAO data, showing the EDE potential construction affects late-time dark energy constraints.
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.
The Hubble tension between local and early-universe expansion-rate measurements may be resolved by early dark energy that speeds up expansion before recombination while satisfying existing constraints.
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Double the axions, half the tension: multi-field early dark energy eases the Hubble tension
Two-field axion-like early dark energy reduces Hubble tension to 1.5 sigma residual and improves high-ell CMB fits over single-field models.
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Running into tension: primordial black holes from ultra-slow-roll inflation, spectral running, and the Hubble tension
EDE models increase inferred α_s from CMB data, strengthening tension with USR PBH models that predict negative running.
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Post-Newtonian Constraints on Scalar-Tensor Gravity
A unified post-Newtonian analysis shows that metric vs Palatini scalar-tensor gravity can yield different γ, β and Yukawa suppression, with Palatini f(R̂) recovering GR’s exterior PN limit for point sources.
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Imprint of swampland-inspired coupled early dark energy
A swampland-inspired DM-EDE coupling is tested against DESI DR2 BAO data, showing the EDE potential construction affects late-time dark energy constraints.
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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.
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The Hubble Tension and Early Dark Energy
The Hubble tension between local and early-universe expansion-rate measurements may be resolved by early dark energy that speeds up expansion before recombination while satisfying existing constraints.