Baryon history and cosmic star formation in non-Gaussian cosmological
  models: numerical simulations
  We present the first numerical, N-body, hydrodynamical, chemical simulations
of cosmic structure formation in the framework of non-Gaussian models. We study
the impact of primordial non-Gaussianities on early chemistry (e, H, H+, H-,
He, He+, He++, H2, H2+, D, D+, HD, HeH+), molecular and atomic gas cooling,
star formation, metal (C, O, Si, Fe, Mg, S) enrichment, population III (popIII)
and population II-I (popII) transition, and on the evolution of "visible"
objects. We find that non-Gaussianities can have some consequences on baryonic
structure formation at very early epochs, but the subsequent evolution at later
times washes out any difference among the various models. When assuming
reasonable values for primordial non-Gaussian perturbations, it turns out that
they are responsible for: (i) altering early molecular fractions in the cold,
dense gas phase of ~10 per cent; (ii) inducing small temperature fluctuations
of <~10 per cent during the cosmic evolution of primordial objects; (iii)
influencing the onset of the first star formation events, at z>~15, and of the
popIII/popII transition of up to some 10^7yr; (iv) determining variations of
<~10 per cent in the gas cloud and stellar mass distributions after the
formation of the first structures; (v) causing only mild variations in the
chemical history of the Universe. We stress, though, that purely non-Gaussian
effects might be difficult to address, since they are strictly twisted with
additional physical phenomena (e.g. primordial gas bulk flows, unknown
primordial popIII stellar mass function, etc.) that have similar or stronger
impact on the behaviour of the baryons.
