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Chameleon Early Dark Energy and the Hubble Tension
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Early dark energy (EDE) offers a particularly interesting theoretical approach to the Hubble tension, albeit one that introduces its own set of challenges, including a new `why then' problem related to the EDE injection time at matter-radiation equality, and a mild worsening of the large-scale structure (LSS) tension. Both these challenges center on the properties of dark matter, which becomes the dominant component of the Universe at EDE injection and is also responsible for seeding LSS. Motivated by this, we present the potential of couplings between EDE and dark matter to address these challenges, focusing on a mechanism similar to chameleon dark energy theories, deeming this chameleon early dark energy (CEDE). We present relevant background and perturbation equations and study the dynamics of the case of a quartic scalar potential and an exponential coupling.
Forward citations
Cited by 12 Pith papers
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A joint CMB, BAO, and supernova fit mildly prefers a non-zero Wald-Gauss-Bonnet dark-energy term (~3σ with SH0ES included), raising H0 from 68.5 to 69.8 km/s/Mpc and easing the Hubble tension by ~0.9σ at the cost of a...
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Hubble tension: the shape wall
Late-time modifications to the expansion history can raise H0 by at most about 2% (conservative) to 3.7% (permissive) if the CMB acoustic scale is fixed.
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The $H_0$ world cup. II. A comprehensive competition between proposed Hubble tension solutions
Against a common 2025-26 dataset (Planck PR4, ACT DR6, SPT-3G, DESI DR2, Pantheon+), early dark energy and early modified gravity models win the H0 competition (~3σ residual tension), while radiation and late-time sol...
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BAO miscalibration cannot rescue late-time solutions to the Hubble tension
Even after rescaling BAO data to prefer H0≈73 km/s/Mpc, none of six tested late-time dark-energy models can resolve the Hubble tension once unanchored SNeIa and CMB geometry are included.
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Searching for coupled, hyperlight scalars across cosmic history
Hyperlight quadratically coupled scalars making up a few percent of dark matter are bounded to near- or sub-gravitational couplings to electrons and photons over 10^-31 to 10^-28 eV, with quasar spectra setting the st...
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The $H_0$ World Cup. I. Summary of the baseline group stage results
In a systematic head-to-head analysis, early dark energy and early modified gravity models reduce the Hubble tension to about 3σ and are favored over ΛCDM, while radiation and late-time alternatives are not.
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Direct detection of solar chameleons with electron recoil data from XENONnT
XENONnT electron-recoil data bound solar chameleons to log10 β_eff < −6.9, independent of the potential index n for inverse power-law chameleons at the dark-energy scale.
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Can the sound horizon-free measurement of $H_0$ constrain early new physics?
Mock galaxy-survey analyses show that sound-horizon-free H0 measurements do not currently rule out BAO-compatible early dark energy models, and LambdaCDM-derived priors can bias the result.
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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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Constraints on Dark Energy Models Using Late Universe Probes
Using late-universe probes only, the authors find all dark energy models remain within 1-2 sigma of Lambda CDM, which wins the Bayesian model comparison, and confirm that DESI's LRG1 and LRG2 points drive the dynamica...
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Effect of Peak Absolute Magnitude of Type Ia Supernovae and Sound Horizon Values on Hubble Tension using DESI results
Using DESI DR1, Pantheon+ and cosmic chronometer data, the authors show that changing the Type Ia supernova absolute magnitude and sound-horizon priors moves the inferred H0 from about 73 to 68 km/s/Mpc, reducing the ...
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The Hubble tension: A decade review
Pure early or late fixes to the Hubble tension are tightly constrained; remaining options are combined early-late interacting dark energy or new physics at the local-to-homogeneous transition.
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