Cosmography has been referred to as a solution to the inverse scattering problem, which is reasonable since it allows us to calculate cosmological bounds from data samples by performing an expansion of the cosmological observables around the present time. Nevertheless, this approach is not properly an inverse scattering solution since the method only circumvents the problem to fit the equation of state (EoS) parameters (model-dependent) by replacing it with their fit of its cosmographic parameters (with a polynomial series-dependence). Therefore, the question that we want to answer is: can we construct a new cosmography approach where the cosmodynamical parameters can be fitted and then employ them to analyse the kinematics via its generic cosmographic parameters? By all means, without experimenting with the traditional problem of truncation of the series that all cosmography proposals in the literature argue. In this work, we present a solution to this question. A generic EoS depending solely on the form of fi(z) and its derivative is found, where this function can be any polynomial (mimicking a dark energy-like term) that allow the dynamics of a specific cosmological density. We test our generic EoS with standard cosmological models and with polynomials proposals as Padé and Chebyshev approximants. All of them reproduce ΛCDM at z>1 between 1-σ, but fail at lower observational redshift range. Interesting enough, a Padé (2,2) approximant has been considered inside a f(z)CDM-like model showing a transition in z=1. Also, we found that this is not assured since models with these characteristics have degeneracy and truncation problems that have a divergence at this redshift limit. With a Chebyshev (2,1) approximant, here proposed, the divergence is not present for large redshifts. To explore our results, also we present a new supernovae sample trained via a deep learning tool called Recurrent-Bayesian (RNN+BNN) network that can solve problems as overfitting at lower redshifts and increase the density of data points in this region, which can help to discern between cosmographies at 2-σ of precision.