  We investigate the redshift (z) evolution of dust properties, its dependences
on initial conditions of galaxy formation, and physical correlations between
dust, gas, and stellar contents at different z based on our original
chemodynamical simulations of galaxy formation with dust growth and
destruction. In this preliminary investigation, we first determine the
reasonable ranges of the most important two parameters for dust evolution,
i.e., the timescales of dust growth and destruction, by comparing the observed
and simulated dust properties and molecular hydrogen H2 content of the Galaxy.
We then investigate the z-evolution of dust-to-gas-ratios (D) and, H2 gas
fraction (f_H2), and gas-phase chemical abundances (e.g., A_O=12+log(O/H)) in
the simulated disk and dwarf galaxies. The principal results are as follows.
Both D and f_H2 can rapidly increase during the early dissipative formation of
galactic disks (z ~ 2-3) and the z-evolution of these depends on initial mass
densities, spin parameters, and masses of galaxies. The observed A_O-D relation
can be qualitatively reproduced, but the simulated dispersion of D at a given
A_O is smaller. The simulated galaxies with larger total dust masses show
larger H2 and stellar masses and higher f_H2. Disk galaxies show negative
radial gradients of D and the gradients are steeper for more massive galaxies.
Both dust-to-metal ratios and gas-phase [S/Fe] can be significantly different
within a single galaxy and between different galaxies at different z, which
means that fixed dust-to-metal ratios should not be used in investigating H2
contents and spectral energy distributions of galaxies.
