A geometric invariance makes the BAO-SN Ω_m gap invariant under sound-horizon rescaling α and requires opposite w(z) deformations for the two datasets, so their combination cannot reach the local H0 value.
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A two-parameter model in which axion dark matter is driven out of equilibrium at late times fits SH0ES and DESI data with H0 ≈ 73 km/s/Mpc, but only when the SH0ES prior is included.
Gravitationally induced particle creation models fit cosmological data as well as ΛCDM and reduce the Hubble tension from 4.3σ to 2.4–3σ.
Cosmographic Taylor and Padé models fitted to Pantheon+SH0ES+GRB+DESI BAO data yield redshift drift predictions compatible with ΛCDM and ω0ω1CDM at 1-2σ, with mock drift data tightening q0 and j0 bounds.
Modified IDE model with interaction parameter alpha ~0.01 from late-universe data shows H0 decreasing with redshift, tightening to 10^-5 when CMB priors are added.
Gravitational vacuum polarization explains the Hubble tension by increasing direct H0 measurements while leaving indirect ones unaffected, does not impact the sigma8 tension, and predicts FRB measurements match CMB/BAO values.
citing papers explorer
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Geometric obstruction to resolving the Hubble tension: orthogonality of scale and shape in distance measurements
A geometric invariance makes the BAO-SN Ω_m gap invariant under sound-horizon rescaling α and requires opposite w(z) deformations for the two datasets, so their combination cannot reach the local H0 value.
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Modifying $\Lambda$CDM dynamics via out-of-equilibrium axions: reconciling SH0ES and DESI $H_0$ values
A two-parameter model in which axion dark matter is driven out of equilibrium at late times fits SH0ES and DESI data with H0 ≈ 73 km/s/Mpc, but only when the SH0ES prior is included.
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Revisiting the Matter Creation Process: Observational Constraints on Gravitationally Induced Dark Energy and the Hubble Tension
Gravitationally induced particle creation models fit cosmological data as well as ΛCDM and reduce the Hubble tension from 4.3σ to 2.4–3σ.
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Mapping the redshift drift at various redshifts through cosmography
Cosmographic Taylor and Padé models fitted to Pantheon+SH0ES+GRB+DESI BAO data yield redshift drift predictions compatible with ΛCDM and ω0ω1CDM at 1-2σ, with mock drift data tightening q0 and j0 bounds.
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Redshift evolution of the Hubble constant: Constraints and new insights from an interacting dark energy model
Modified IDE model with interaction parameter alpha ~0.01 from late-universe data shows H0 decreasing with redshift, tightening to 10^-5 when CMB priors are added.
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Gravitational particle production, the cosmological tensions and fast radio bursts
Gravitational vacuum polarization explains the Hubble tension by increasing direct H0 measurements while leaving indirect ones unaffected, does not impact the sigma8 tension, and predicts FRB measurements match CMB/BAO values.