Papers › A w-M phantom transition at zₜ<0.1 as a resolution of the Hubble tension
A w-M phantom transition at zₜ<0.1 as a resolution of the Hubble tension
George Alestas, Lavrentios Kazantzidis, Leandros Perivolaropoulos
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A rapid phantom transition of the dark energy equation of state parameter w at a transition redshift zₜ<0.1 of the form w(z)=-1+Δw Θ(zₜ-z) with Δw<0 can lead to a higher value of the Hubble constant while closely mimicking a Planck18/ΛCDM form of the comoving distance r(z)=∫₀ᶻ(dz′)/(H(z′)) for z>zₜ. 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 H₀ 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+ΔM Θ(z-zₜ) with ΔM<0. This is a Late w-M phantom transition (LwMPT). It may be achieved by a sudden reduction of the value of the normalized effective Newton constant μ=G_(eff)/G_N by about 6% assuming that the absolute luminosity of SnIa is proportional to the Chandrasekhar mass which varies as μ^(-3/2). 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 zₜ=0.02 we find Δw≃-4, ΔM ≃-0.1. This model also addresses the growth tension due to the predicted lower value of μ at z>zₜ. A prior of Δw=0 (no w transition) can still resolve the H₀ tension with a larger amplitude M transition with ΔM≃-0.2 at zₜ≃0.01. This implies a larger reduction of μ for z>0.01 (about 12%). 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 μ=1 at z<0.01.
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