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Chameleon dark energy can resolve the Hubble tension
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abstract
Values of the Hubble constant between the direct measurements from various independent local observations and that inferred from the cosmic microwave background with the $\Lambda$-cold-dark-matter model are in tension with persistent significance. We propose a late-time inhomogeneous resolution suggesting that a chameleon field coupled to a local overdensity of matter could be trapped at a higher potential energy density as an effective cosmological constant driving the local expansion rate faster than that of the background with lower matter density. We illustrate this mechanism in a toy model in which a region with only $20\%$ overdensity of matter is sufficient to resolve the Hubble tension, and the Hubble constant measured by the local distance ladders could be accommodated by the chameleon coupled to the observed overdensities from the large-scale structure surveys.
Forward citations
Cited by 7 Pith papers
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Direct detection of solar chameleons with electron recoil data from XENONnT
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With DESI DR2 BAO plus CMB and a SH0ES prior, the two-parameter eeΛCDM model gives δΛ=-0.41±0.14 and H0=71.9±1.0, easing the Hubble tension to 0.8σ, but SN datasets erase the signal.
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An overview of what current data can (and cannot yet) say about evolving dark energy
The apparent preference for evolving dark energy depends strongly on which supernova catalog and which BAO survey are used, and is not robust across all independent data combinations.
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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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Interacting Early Dark Energy
The paper derives a modified radiation scaling and a decaying field-to-radiation ratio for an exponentially coupled scalar, but the claimed cosmological constant behavior and data agreement are not supported.
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