Lorentzian Quintessential Inflation
  From the assumption that the slow roll parameter $\epsilon$ has a Lorentzian
form as a function of the e-folds number $N$, a successful model of a
quintessential inflation is obtained. The form corresponds to the vacuum energy
both in the inflationary and in the dark energy epochs. The form satisfies the
condition to climb from small values of $\epsilon$ to $1$ at the end of the
inflationary epoch. At the late universe $\epsilon$ becomes small again and
this leads to the Dark Energy epoch. The observables that the models predicts
fits with the latest Planck data: $r \sim 10^{-3}, n_s \approx 0.965$.
Naturally a large dimensionless factor that exponentially amplifies the
inflationary scale and exponentially suppresses the dark energy scale appears,
producing a sort of {\it{cosmological see saw mechanism}}. We find the
corresponding scalar Quintessential Inflationary potential with two flat
regions - one inflationary and one as a dark energy with slow roll behavior.
