evolutionary spectral synthesis model for starbursts and evolved galaxies of the Hubble sequence. It is continuous over an exceptionally large wavelength range from 220 Å  up to 5$\mu$m. It was extended to the NIR of the atlas of synthetic spectra of Rocca-Volmerange & Guiderdoni (1988) with a revised stellar library including cold star parameters and stellar tracks extended to the thermally-pulsing regime of the asymptotic giant branch (TP-AGB) and the post-AGB phase. The synthetic stellar spectral library is taken from Kurucz (1992), modified by Lejeune et al. (1997) to fit the observed colors. A set of reference synthetic spectra at z = 0, to which the cosmological k- and evolution e- corrections for high-redshift galaxies are applied, is built from fits of observational templates (Fioc & Rocca-Volmerange 1997).

With the PEGASE code, we can compute the stellar SEDs of starbursts and evolved galaxies of the Hubble sequence at any stage of evolution, within the metallicity range Z = 10$^{-4}$ to 10$^{-1}$. Typical parameters of PEGASE are the star formation rate (SFR) and IMF. Assuming a standard IMF, SFR and other initial conditions, such as dust extinction, the PEGASE code will give an evolutionary history and some other important properties of 