  The main aim of this paper is to perform a model comparison for some
reconstructions of the key properties that describe the dark energy of the
Universe i.e. energy density and the equation of state (EoS). We carry out this
process by using a binning and a linear interpolation methodologies, and on top
of that, we incorporate a correlation function mechanism. An extension of the
two of them was also introduced, where internal amplitudes are allowed to vary
in height as well as in position. The reconstructions were made with data from
the Hubble parameter, Supernovae Type Ia and Baryon Acoustic Oscillations
(H+SN+BAO), all of which span a range from $z=0.01$ to $z=2.34$. First we
perform the parameter estimation for each of the reconstructions to then
provide a model selection through the Bayesian Evidence. Throughout our process
we found a better fit to the data, up to $4\sigma$ compared to $\Lambda$CDM,
and the presence of some interesting features, i.e. an oscillatory behaviour at
late times, a decrease in the dark energy density component at early times and
a transition to the phantom divide-line in the EoS. To discern these features
from noisy contributions, we include a principal component analysis and found
that some of these characteristics should be taken into account to satisfy
current observations.
