  We present the first results of a detailed modeling of chemical and
photometric evolution of galaxies including the effects of a dusty interstellar
medium. A chemical evolution code follows the SF rate, the gas fraction and the
metallicity, basic ingredients for the stellar population synthesis. The latter
is performed with a grid of integrated spectra for SSP of different ages and
metallicities, in which the effects of dusty envelopes around AGB stellar are
included. The residual fraction of gas in the galaxy is divided into two
phases: the star forming molecular clouds and the diffuse medium. The molecular
gas is sub-divided into clouds of given mass and radius: it is supposed that
any SSP is borne within the cloud and progressively escapes it. The emitted
spectrum of the star forming molecular clouds is computed with a radiative
transfer code. The diffuse dust emission (cirrus) is derived by describing the
galaxy as an axially symmetric system, in which the local dust emissivity is
consistently calculated as a function of the local field intensity due to the
stellar component. Effects of very small grains, subject to temperature
fluctuations, as well as PAH are included. The model is compared and calibrated
with available data of starburst galaxies in the local universe, in particular
new broad-band and spectroscopic ISO observations. It will be a fundamental
tool to extract information on global evolution of the stellar component and of
ISM of galaxies from observations covering four decades in $\lambda$. The
combination of observations from HST, Keck, ISO and ground-based optical, IR
and sub-mm telescopes already provided several objects at relevant $z$ with
spectral information on this large $\lambda$ range. Their number will increase
after the completion of ISO surveys, and will burst when SIRFT, FIRST, Planck
