light in far IR radiation. In brief the @Piovan06b model follows the infall scheme, allows for the onset of galactic winds, and contains three main components: (i) the diffuse interstellar medium composed of gas and dust whose emission and extinction properties have been studied in detail by @Piovan06a, (ii) the large complexes of molecular clouds in which new stars are formed and (iii) the stars of any age and chemical composition. The total gas and star mass provided by the chemical model are distributed over the whole volume by means of suitable density profiles, one for each component and depending on the galaxy type (spheroidal, disk and disk plus bulge). The galaxy is then splitted in suitable volume elements to each of which the appropriate amounts of stars, molecular clouds and interstellar medium are assigned. Each elemental volume absorbs radiation from all other volumes and from the interstellar medium in between. The elemental volume also re-emits the absorbed light and produces radiation by the stars that it contains. On the other hand, the star formation, the initial mass function, the chemical enrichment of the @Piovan06b model are much similar to those by @Bressan94 [@Tantalo96; @Tantalo98; @Portinari98].

Coupling dynamical simulations and 