All Tables

Table 1: Features of the examined models: in order, bulge mass, star formation efficiency, bulge effective radius. The table also reports the time of occurrence of the galactic wind.
Table 2: Values assumed by the chemical abundance ratios and by the metallicity in solar units after the wind by bulges of different masses, and the time by which $Z_{\odot }$ is reached in the different models (last line).
Table 3: Predicted colours for the Galactic bulge assuming two different IMFs, compared to observational values of local bulges from various sources (a: Balcells & Peletier 1994; b: Galaz et al. 2006).