Stellar tracks

The stellar tracks are grouped in files named according to the following conventions: modIzzz.ext, where I stands for the database ID (col. 2, Table ), zzz for the metallicity, and ext for the extension specifying the type of data (see Table ). For example modc001.WFPC2 contains the WFPC2 photometric data for all stellar tracks of the model grid # 2.

Grids 1-16 are included integrally in the database. The files with the ID ``c'' or ``e'' contain the 1.25 M_ M$_{\odot}$ track calculated with overshooting. The corresponding no overshoot model is found in the ``o'' files, as indicated in col. 9 of Table . The ``l'' model set, providing the most appropriate low mass star models, consist of the following combination of tracks: 0.4-1 M_ M$_{\odot}$ main sequence tracks from paper VIII (grids 15, 17 respectively), post-He flash models for 0.9 and 1 M_ M$_{\odot}$ from paper VI (with ages properly adjusted to the calculations of paper VIII), 1.25 (no overshoot), 1.5, and 1.7 M_ M$_{\odot}$ tracks from paper VI (grids 13, 14 respectively), and 2 and 2.5 M_ M$_{\odot}$ tracks from paper I (grids 2, 5).

Obviously some of the sets in the database contain redundant data. This is due to the organisation of the sets designed for a simple and covenient use. See Section for some recommendations on how to use the database.

Figure: Synthetic colour-magnitude diagrams in different observationnal planes (upper left: Johnson, upper right: HST-WFPC2, lower left: Geneva, lower right: Washington system) for the Gyr isochrones at different metallicities: from left to right in each panel, 0.0004, 0.001, 0.004, 0.008, 0.02, 0.04, and 0.1 (dashed line).

The content of the various files is as follows:

• *.dat files: Predicted surface stellar properties using the table format described in paper I (column 1-15), complemented by the stellar core temperature for Wolf-Rayet stars or otherwise (col. 16), and the mass loss rate ( in M_ M$_{\odot}$/yr; col. 17). Column 1-15 contain the following values: ID of evolutionary point (col. 1), age (2), present mass (3), (4), (5), and the surface abundances in mass fraction of H, He, C, C, N, O, O, O, Ne, and Ne (cols. 6-15). The central properties are given in the tables of the original papers.

• *.UBVRIJHKLM files: ID of evolutionary point (col. 1), age (2), present mass (3), (4), (5), (6), (7), (8), (9), (10), (11), (12), (13), (14), (15), (16), (17), (18), (19), (20), (21).

• *.WFPC2 files: ID of evolutionary point (col. 1), age (2), present mass (3), (4), (5), (6), (7), F336W-F439W (8), F439W-F555W (9), F555W-F675W (10), F555W-F814W (11), F675W-F814W (12), F439W- (13).

• *.geneva files: ID of evolutionary point (col. 1), age (2), present mass (3), (4), (5), (6), (7), (8), (9), (10), (11), (12), (13), (14), (15), (16), (17).

• *.CMT1T2 files: ID of evolutionary point (col. 1), age (2), present mass (3), (4), (5), (6), (7), (8), (9), (10), (11), (12), (13), (14), (15), (16).