Theoretical clues about dust accumulation and galaxy obscuration at high
  and low redshift
  Since the epoch of cosmic star formation peak at $z \sim 2$, most of it is
obscured in high mass galaxies, while in low mass galaxies the radiation
escapes unobstructed. During the reionization epoch, the presence of evolved,
dust obscured galaxies are a challenge to galaxy formation and evolution
models. By means of a chemodynamical evolution model, we investigate the star
formation and dust production required to build up the bulk of dust in galaxies
with initial baryonic mass ranging from $7.5 \times 10^{7}$~M$_\odot$ to $2.0
\times 10^{12}$~M$_\odot$. The star formation efficiency was also chosen to
represent the star formation rate from irregular dwarf to giant elliptical
galaxies. We adopted a dust coagulation efficiency from \citep[][Case
A]{dwek1998evolution} as well as a lower efficiency one (Case B), about five
times smaller than Case A. All possible combination of these parameters was
computed, summing forty different scenarios. We find that in high stellar
formation systems the dust accretion in ISM rules over stellar production
before the star formation peak, making these systems almost insensible to dust
coagulation efficiency. In low star formation systems, the difference between
Case A and B lasts longer, mainly in small galaxies. Thus, small irregular
galaxies should be the best place to discriminate different dust sources. In
our observational sample, taken from the literature, dust-to-gas ratio tends to
be more spread only than dust mass, for both stellar mass and star formation
rate. Dust-to-gas vs. dust-to-star diagram is a good tracer for both galaxy and
dust evolution, due to the link between gas, star, dust and star formation
rate. However, the model do not constrain simultaneously all this quantities.
The new generation facilities (such as JWST, ELT, VLT and SPICA) will be
indispensable to constrain dust formation across the cosmic time.
