last modification: 18 feb 2011
This database contains the grid of evolutionary pre main-sequence tracks described in Pietrinferni, Cassisi, Salaris & Castelli (2004, ApJ, 612, 168) and in Pietrinferni, Cassisi, Salaris and Castelli (2006, ApJ - vol. 642, 797).
The models do not include gravitational settling, radiative acceleration, convective overshooting, rotational mixing, but otherwise they are based on up-to-date physics, as detailed in the quoted paper. We have presently stored evolutionary models with the following chemical compositions:
The values Z=0.0198 (zsun) and Y=0.2734 (ysun) correspond to the abundances obtained from the calibration of the solar model (for more details we refer to Pietrinferni et al. 2004).
Each file contains:
in the fifth line - 1) the number of evolutionary points, 2) the global metallicity [M/H], 3) the abundance by mass of metals (Z), 4) the initial He abundance (Y), 5) the inital mass (in solar unit); starting from the ninth line the following quantities are listed:
1 column) the logarithm of the age in years; 2 column) the actual mass in solar unit; 3 column) the logarithm of the surface luminosity in solar unit; 4 column) the logarithm of the effective temperature (K); 5 column) the visual absolute magnitude; 6 column) the (B-V) colour; 7 column) the (U-B) colour; 8 column) the (V-I) colour; 9 column) the (V-R) colour; 10 column) the (V-J) colour; 11 column) the (V-K) colour; 12 column) the (V-L) colour; 13 column) the (H-K) colour;from the first model until the Zero Age main Sequence. For details about the adopted colour - effective temperature relations and bolometric correction scale we refer to the quoted reference.
The coding of the file names is as follows:
abcdZedfYghis.npr_c03hbs | | evolutionary track for a model with --> initial mass = ab.cd Mo --> metallicity Z= e.d x 10^(-f) --> initial He abundance Y = 0.ghi
The full set of evolutionary tracks can be also downloaded as a single compressed tar archive.
The whole set of evolutionary models has been also transferred from the theoretical plane to the WFC3 (IR) on board of HST. Each set of models can be downloaded as a single compressed tar archive. Each file contains:
on the fifth line - 1) the number of evolutionary points, 2) the global metallicity [M/H], 3) the abundance by mass of metals (Z), 4) the initial He abundance (Y), 5) the inital mass (in solar unit); starting from the ninth line the following quantities are listed, :
1 column) the logarithm of the age in years; 2 column) the actual mass in solar units; 3 column) the logarithm of the surface luminosity in solar units; 4 column) the logarithm of the effective temperature (K); 5 column) F098M magnitude; 6 column) F105W magnitude; 7 column) F110W magnitude; 8 column) F125W magnitude; 9 column) F126N magnitude; 10 column) F127M magnitude; 11 column) F128N magnitude; 12 column) F130N magnitude; 13 column) F132N magnitude; 14 column) F139M magnitude; 15 column) F140W magnitude; 16 column) F153M magnitude; 17 column) F160W magnitude; 18 column) F164N magnitude; 19 column) F167N magnitude;
As for the choice of the key stages, we provide some information in the following.
In order to obtain an accurate sampling of the evolutionary pre main-sequence tracks morphology, we have accounted for 4 key stages along the track, more in detail:
The correspondence between key stages and rows is the following:
For more details about the adopted key stages, please contact one of the authors.
In case one is interested in the complete evolutionary track (i.e, a non normalized track) as well as to more information about the models (such as burnings, internal structure and so on) we will be pleased to provide them upon request. All comments/suggestions/requests are welcome. We hope that this database will be useful to your work!
Our best regards!!!