We have carried out a complete analysis of the kinematics and the stellar populations of the double-barred S0 galaxy NGC 357. We have measured suitable absorption line strength indices on very high quality spectra. With the aid of stellar population models we have obtained the relative ages and metallicities for the different components to constrain the star formation history of this galaxy and test whether the nuclear bar is transporting gas to the central regions of the galaxy efficiently enough to trigger star formation. Our first results indicate that the bulk of the stellar populations of NGC 357 was completely formed in less than 1 Gyr. The old ages obtained for both the bulge and the nuclear bar indicate that the latter is not playing an important role in fueling the star formation in the center.