For most purposes the ``basic model set'' (files with the ID ``c'') should be appropriate. The tracks of this set have e.g. been applied to analysis of Galactic open clusters with ages 4 Myr - 9.5 Gyr by Meynet et al. (1993).
For analysis of massive stars ( _) the high mass loss models (ID: ``e'') should preferrentially be used (see Maeder & Meynet 1994).
For studies of low mass stars ( 0.4 - 2.5 M_ M) the combined model set (ID: ``l'') at Z=0.001 and Z=0.02 should be most appropriate since it includes the MHD equation of state for 1 M_ M and covers also the post-Helium flash evolutionary phases of stars with masses 0.8 _ 1.7.
For studies limited to the lowest masses ( 1 M_ M) the ``m'' set should be preferred.
For studies critical to the properties of stars in the mass range 1. - 1.5 M_ M, corresponding to the appearance of core convection on the main sequence, the ``o'' sets allow in comparison with the basic sets (``c'') to study the effect of enhanced convective cores (overshooting) in this mass range.
As mentioned earlier, the Geneva stellar grids used in this work do not include thermally pulsing AGB stars and post-AGB phases, such as central stars of planetary nebulae (CSPN) and white dwarfs (WD). If necessary the present data must be complemented with existing calculations from the literature. For recent calculations of AGB stars we refer e.g. to the complete or combined complete + synthetic models of Vassiliadis & Wood (1993), Blöcker (1995a), Forestini & Charbonnel (1997), and Langer et al. (1999), and to the synthetic models of Van den Hoeck & Groenewegen (1997) and Marigo et al. (1998). Recent models of CSPN and WD are given by e.g. Blöcker (1995b) Driebe et al. (1998), and Hansen & Phinney (1998).