The interstellar dust is acquiring a primary role in the fascinating subject of the origin and evolution of galaxies, because of its growing importance in: (1) the observations of the high-z Universe (Omont et al. 2001; Shapley et al. 2001; Bertoldi et al. 2003; Robson et al. 2004; Wang et al. 2008; Gallerani et al. 2010; Michalowski et al. 2010a,b; Dayal et al. 2012) and (2) the theoretical spectro-photometric, dynamical, and chemical modelling of galaxies (Narayanan et al. 2010; Jonsson et al. 2010; Grassi et al. 2010; Pipino et al. 2011; Popescu et al. 2011). Dust absorbs the stellar radiation in the UV/optical range of the electromagnetic spectrum and re-emits it in the IR, deeply changing the shape of the observed spectral energy distributions (SEDs) of obscured galaxies (Silva et al. 1998; Piovan et al. 2006a,b; Popescu et al. 2011). Only taking into account all the spectral range of emission it is possible to study the properties of galaxies by means of the evolutionary population synthesis (EPS) models. It is therefore mandatory to calculate evolutionary sequences of spectral models for galaxies of various morphological types, including the effects of dust, both for the local and high redshift objects. The comparison between models with observations allow to constrain the parameters used to calculate the galactic SEDs and to get clues about the evolution of galaxies by means of the EPS method.