The $H_0$ tension: $ΔG_N$ vs. $ΔN_{\rm eff}$

Abstract: We investigate whether the $4.4\sigma$ tension on $H_0$ between SH${0}$ES 2019 and Planck 2018 can be alleviated by a variation of Newton's constant $G_N$ between the early and the late Universe. This changes the Hubble rate before recombination, similarly to adding $\Delta N{\rm eff}$ extra relativistic degrees of freedom. We implement a varying $G_N$ in a scalar-tensor theory of gravity, with a non-minimal coupling $(M^2+\beta \phi^2)R$. If the scalar $\phi$ starts in the radiation era at an initial value $\phi_I \sim 0.5~M_p$ and with $\beta<0$, a dynamical transition occurs naturally around the epoch of matter-radiation equality and the field evolves towards zero at late times. As a consequence, the $H_0$ tension between SH${0}$ES (2019) and Planck 2018+BAO slightly decreases, as in $\Delta N{\rm eff}$ models, to the 3.8$\sigma$ level. We then perform a fit to a combined Planck, BAO and supernovae (SH$0$ES and Pantheon) dataset. When including local constraints on Post-Newtonian (PN) parameters, we find $H_0=69.08{-0.71}^{+0.6}~\text{km/s/Mpc}$ and a marginal improvement of $\Delta\chi^2\simeq-3.2$ compared to $\Lambda$CDM, at the cost of 2 extra parameters. In order to take into account scenarios where local constraints could be evaded, we also perform a fit without PN constraints and find $H_0=69.65_{-0.78}^{+0.8}~\text{km/s/Mpc}$ and a more significant improvement $\Delta\chi^2=-5.4$ with 2 extra parameters. For comparison, we find that the $\Delta N_{\rm eff}$ model gives $H_0=70.08_{-0.95}^{+0.91}~\text{km/s/Mpc}$ and $\Delta\chi^2=-3.4$ at the cost of one extra parameter, which disfavors the $\Lambda$CDM limit just above 2$\sigma$, since $\Delta N_{\rm eff}=0.34_{-0.16}^{+0.15}$. Overall, our varying $G_N$ model performs similarly to the $\Delta N_{\rm eff}$ model in respect to the $H_0$ tension, if a physical mechanism to remove PN constraints can be implemented.