  In quintessence scalar field theories, the presence of scaling solutions are
important during the radiation and matter epoch due to having their attractor
character. Usually, it is assumed that the initial conditions of the
quintessence field are in the basin of attraction of the scaling solutions.
However, in order to reproduce the current cosmic acceleration, at late times,
a mechanism to exit this behavior is needed. In the present work we show that
the quintessential inflation models could be an excellent candidate to exhibit
the above behavior. However, the crucial point of quintessential inflation is
that the initial conditions has to be taken during the inflation, and at the
beginning of the radiation era, the scalar field does not belong to the basin
of attraction of the scaling solution. This means that, in the case where
quintessence is depicted via exponential potentials, only a single exponential
in the tail of the { quintessential inflation} potential is enough to depict
the evolution of our universe.
