Modelling galaxy spectra in presence of interstellar dust-III. From
  nearby galaxies to the distant Universe
  Improving upon the standard evolutionary population synthesis (EPS)
technique, we present spectrophotometric models of galaxies whose morphology
goes from spherical structures to discs, properly accounting for the effect of
dust in the interstellar medium (ISM). These models enclose three main physical
components: the diffuse ISM composed by gas and dust, the complexes of
molecular clouds (MCs) where active star formation occurs and the stars of any
age and chemical composition. These models are based on robust evolutionary
chemical models that provide the total amount of gas and stars present at any
age and that are adjusted in order to match the gross properties of galaxies of
different morphological type. We have employed the results for the properties
of the ISM presented in Piovan, Tantalo & Chiosi (2006a) and the single stellar
populations calculated by Cassar\`a et al. (2013) to derive the spectral energy
distributions (SEDs) of galaxies going from pure bulge to discs passing through
a number of composite systems with different combinations of the two
components. The first part of the paper is devoted to recall the technical
details of the method and the basic relations driving the interaction between
the physical components of the galaxy. Then, the main parameters are examined
and their effects on the spectral energy distribution of three prototype
galaxies are highlighted. We conclude analyzing the capability of our galaxy
models in reproducing the SEDs of real galaxies in the Local Universe and as a
function of redshift.
