  The impacts of Compton scattering of hot cosmic gas with the cosmic microwave
background radiation (Sunyaev-Zel'dovich effect, SZ) are consistently
quantified in Gaussian and non-Gaussian scenarios, by means of 3D numerical,
N-body, hydrodynamic simulations, including cooling, star formation, stellar
evolution and metal pollution (He, C, O, Si, Fe, S, Mg, etc.) from different
stellar phases, according to proper yields for individual metal species and
mass-dependent stellar lifetimes. Light cones are built through the simulation
outputs and samples of one hundred maps for the resulting temperature
fluctuations are derived for both Gaussian and non-Gaussian primordial
perturbations. From them, we estimate the possible changes due to early
non-Gaussianities on: SZ maps, probability distribution functions, angular
power spectra and corresponding bispectra. We find that the different growth of
structures in the different cases induces significant spectral distortions only
in models with large non-Gaussian parameters, $f_{\rm NL}$. In general, the
overall trends are covered by the non-linear, baryonic evolution, whose
feedback mechanisms tend to randomize the gas behaviour and homogenize its
statistical features, quite independently from the background matter
distribution. Deviations due to non-Gaussianity are almost undistinguishable
for $f_{\rm NL}\lesssim 100$, remaining always at few-per-cent level, within
the error bars of the Gaussian scenario. Rather extreme models with $f_{\rm
NL}\sim1000$ present more substantial deviations from the Gaussian case,
overcoming baryon contaminations and showing discrepancies up to a factor of a
few in the spectral properties.
