  In this work, we study the effects on the relevant observational parameters
of an inflationary universe from a chaotic potential with a step. We
numerically evolve the perturbation equations within both cold inflation and
warm inflation. On the one hand, in a cold inflation scenario we analyse the
scalar power spectrum $P_{\mathcal{R}}$ in terms of the number of e-folds
$N_{e}$, and in terms of the ratio $k/k_{0}$, where $k_{0}$ is our pivot scale.
We show how $P_{\mathcal{R}}$ oscillates around $0.2< k/k_{0} < 20$.
Additionally, we present the evolution of two relevant parameters: the scalar
spectral index $n_\mathrm{s}$ and the tensor-to-scalar ratio $r$. In fact, more
than one region of $(n_\mathrm{s},r)$ lies within the observable window (Planck
2018). On the other hand, in the warm inflationary case, we also examine the
evolution of $P_{\mathcal{R}}$ in terms of $N_{e}$ and $k/k_{0}$. Perturbations
are amplified in WI; in fact, $P_{\mathcal{R}}$ can be much larger than the CMB
value $P_{\mathcal{R}}> 2.22\times 10^{-9}$. This time, the spectral index
$n_\mathrm{s}$ is clearly blue-tilted, at smaller scales, and the
tensor-to-scalar ratio $r$ becomes too low. However, $n_\mathrm{s}$ can change
from blue-tilted towards red-tilted, since $P_{\mathcal{R}}$ starts oscillating
around $k/k_{0}\sim 40$. Indeed, the result from the step potential skims the
Planck contours. Finally, one key aspect of this research was to contrast the
features of an inflationary potential between both paradigms, and, in fact,
they show similarities and differences. Due to a featured background and a
combined effect of entropy fluctuations (only in warm inflation), in both
scenarios certain fluctuation scales are not longer ``freeze in'' on
super-horizon scales.
