H 0 tension as a hint for a transition in gravitational theory

作者： Nima Khosravi , Shant Baghram , Niayesh Afshordi , Natacha Altamirano

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摘要: We propose a cosmological model, $\"u\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$, based on ``\"uber gravity,'' which is canonical ensemble average of many theories gravity. In this we have sharp transition from (a purely) $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ era to phase in the Ricci scalar constant. This occurs when reaches critical scale or alternatively redshift, ${z}_{\ensuremath{\bigoplus}}$. use observations baryonic acoustic oscillations and supernovae Ia, as well cosmic microwave background data constrain $\"u\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$. yields ${H}_{0}={70.6}_{\ensuremath{-}1.3}^{+1.1}\text{ }\text{ }\mathrm{km}/\mathrm{s}/\mathrm{Mpc}$, ${\mathrm{\ensuremath{\Omega}}}_{m}=0.2861\ifmmode\pm\else\textpm\fi{}0.0092$, ${z}_{\ensuremath{\bigoplus}}=0.53{7}_{\ensuremath{-}0.375}^{+0.277}$, providing marginally better fit with Akaike information criterion 0.8. Therefore, $\"u\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ can ease ${H}_{0}$ tension, albeit marginally, one additional free parameter. also provide preliminary study linear perturbation theory that points interesting potential smoking guns large structure at $zl{z}_{\ensuremath{\bigoplus}}$.

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H 0 tension as a hint for a transition in gravitational theory

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H 0 tension as a hint for a transition in gravitational theory

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