Model-independent reconstruction of $f(T)$ teleparallel cosmology

Understand

We propose a model-independent formalism to numerically solve the modified Friedmann equations in the framework of $f(T)$ teleparallel cosmology.

• Our strategy is to expand the Hubble parameter around the redshift $z=0$ up to a given order and to adopt cosmographic bounds as initial settings to determine the corresponding $f(z)\equiv f(T(H(z)))$ function.
• In this perspective, we distinguish two cases: the first expansion is up to the jerk parameter, the second expansion is up to the snap parameter.
• We show that inside the observed redshift domain $z\leq1$, only the net strength of $f(z)$ is modified passing from jerk to snap, whereas its functional behavior and shape turn out to be identical.