The current compilation includes all grids of Geneva stellar evolution models published between 1992 and march 1999 in papers I-VIII (references here) and a new grid of stellar models for very low metallicity (Z=1/50 Z/Z, see Appendix). Pre-main sequence models are not included (but cf. Bernasconi 1996 and paper VIII).
The conversion of the theoretical tracks and isochrones of the present compilation to observational colour-magnitude (c-m) diagrams has been performed using the stellar spectral library, BaSeL-2.2 of Lejeune et al. (1997, 1998) and Westera et al. (1999), that provides empirically and semi-empirically colour-calibrated model atmosphere spectra for a large range of fundamental stellar parameters, (2000 K to 50,000 K), (-1.0 to 5.5), and (5.0 to +1.0).
In order to transform the theoretical quantities (L,Teff) into magnitudes and colours, we first compute, by interpolation in the Ba Se L grid (Teff, logg, [Fe/H]; the solar metallicity [Fe/H]=0 is identified with the Z=0.02 tracks. For other metallicities, we adopt the relation [Fe/H]=log(Z/Zsun) with Zsun= 0.02) the model spectrum at each point along the track or the isochrone, and then derive the synthetic photometry by convolving the resulting flux distribution with the filter transmission functions (as given in the following sections).