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Improving upon the standard evolutionary population synthesis (EPS)technique, we present spectrophotometric models of galaxies whose morphologygoes from spherical structures to discs, properly accounting for the effect ofdust in the interstellar medium (ISM). These models enclose three main physicalcomponents: the diffuse ISM composed by gas and dust, the complexes ofmolecular clouds (MCs) where active star formation occurs and the stars of anyage and chemical composition. These models are based on robust evolutionarychemical models that provide the total amount of gas and stars present at anyage and that are adjusted in order to match the gross properties of galaxies ofdifferent morphological type. We have employed the results for the propertiesof the ISM presented in Piovan, Tantalo & Chiosi (2006a) and the single stellarpopulations calculated by Cassar\`a et al. (2013) to derive the spectral energydistributions (SEDs) of galaxies going from pure bulge to discs passing througha number of composite systems with different combinations of the twocomponents. The first part of the paper is devoted to recall the technicaldetails of the method and the basic relations driving the interaction betweenthe physical components of the galaxy. Then, the main parameters are examinedand their effects on the spectral energy distribution of three prototypegalaxies are highlighted. We conclude analyzing the capability of our galaxymodels in reproducing the SEDs of real galaxies in the Local Universe and as afunction of redshift.

Modelling galaxy spectra in presence of interstellar dust-III. From nearby galaxies to the distant Universe