“Researchers at Johns Hopkins University and Swarthmore College have recently proposed and tested an alternative model that could solve the Hubble tension.”
“The researchers successfully applied a model of dark energy previously presented by Marc Kamionkowski (one of the authors), which describes it as evolving but non-interactive to the Hubble tension.”
The original research published at Phys. Rev. Lett:
Early Dark Energy can Resolve the Hubble Tension
Vivian Poulin, Tristan L. Smith, Tanvi Karwal, and Marc Kamionkowski
Phys. Rev. Lett. 122, 221301 – Published 4 June 2019
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Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, Maryland 21218, USA
Department of Physics and Astronomy, Swarthmore College, 500 College Avenue, Swarthmore, Pennsylvania 19081, USA
ABSTRACT
Early dark energy (EDE) that behaves like a cosmological constant at early times (redshifts z≳3000) and then dilutes away like radiation or faster at later times can solve the Hubble tension. In these models, the sound horizon at decoupling is reduced resulting in a larger value of the Hubble parameter H_0 inferred from the cosmic microwave background (CMB). We consider two physical models for this EDE, one involving an oscillating scalar field and another a slowly rolling field. We perform a detailed calculation of the evolution of perturbations in these models. A Markov Chain Monte Carlo search of the parameter space for the EDE parameters, in conjunction with the standard cosmological parameters, identifies regions in which H0 inferred from Planck CMB data agrees with the SH0ES local measurement. In these cosmologies, current baryon acoustic oscillation and supernova data are described as successfully as in the cold dark matter model with a cosmological constant, while the fit to Planck data is slightly improved. Future CMB and large-scale-structure surveys will further probe this scenario.
https://arxiv.org/pdf/1811.04083.pdf
https://phys.org/news/2019-06-early-dark-energy-hubble-tension.html
https://journals.aps.org/prl/abstract/10.1103/PhysRevLett.122.221301