A $w-M$ phantom transition at $z_t<0.1$ as a resolution of the Hubble tension

A rapid phantom transition of the dark energy equation of state parameter $w$ at a transition redshift $z_t<0.1$ of the form $w(z)=-1+\Delta w;\Theta (z_t-z)$with$\Delta w<0$ can lead to a higher value of the Hubble constant while closely mimicking a Planck18/$\mathrm{\Lambda }$CDM form of the comoving distance $r(z)={\int }_0^z\frac{d{z}^{\mathrm{\prime }}}{H(z^{\mathrm{\prime }})}$ for $z>z_t$. Such a transition however would imply a significantly lower value of the SnIa absolute magnitude $M$ than the value $M_C$ imposed by local Cepheid calibrators at $z<0.01$. Thus, in order to resolve the $H_0$ tension it would need to be accompanied by a similar transition in the value of the SnIa absolute magnitude $M$ as $M(z)=M_C+\Delta M ;\Theta (z-z_t)$with$\Delta M<0$\mathrm{.}ThisisaLate$w-M$ phantom transition ($LwMPT$). It may be achieved by a sudden reduction of the value of the normalized effective Newton constant $\mu =G_{\mathrm{e}\mathrm{f}\mathrm{f}}\mathrm{/}{G}_{\mathrm{N}}$ by about $6\mathrm{\%}$ assuming that the absolute luminosity of SnIa is proportional to the Chandrasekhar mass which varies as ${\mu }^{-3\mathrm{/}2}$. We demonstrate that such an ultra low $z$ abrupt feature of $w-M$ provides a better fit to cosmological data compared to smooth late time deformations of $H(z)$ that also address the Hubble tension. For $z_t=0.02$ we find $\mathrm{\Delta }w\simeq -4$, $\Delta M \simeq -0.1$. This model also addresses the growth tension due to the predicted lower value of $\mu$ at $z>z_t$. A prior of $\mathrm{\Delta }w=0$ (no $w$ transition) can still resolve the $H_0$ tension with a larger amplitude $M$ transition with $\mathrm{\Delta }M\simeq -0.2$ at $z_t\simeq 0.01$. This implies a larger reduction of $\mu$ for $z>0.01$ (about $12\mathrm{\%}$). The $LwMPT$ can be generically induced by a scalar field non-minimally coupled to gravity with no need of a screening mechanism since in this model $\mu =1$ at $z<0.01$.