************************************************************ ************************************************************ ** TABLES OF ISOCHRONES WITH IMPROVED TP-AGB MODELS ** ************************************************************ ************************************************************ This directory contains the data files described in the appendix of "Coupling emitted light and chemical yields from stars: a basic constraint to population synthesis models of galaxies " by Paola Marigo and Leo Girardi, (2001), to appear in Astronomy and Astrophysics (astro-ph/0107563). Please refer to this paper for a complete description of the models. ******************************************************** TABLES OF ISOCHRONES (see APPENDIX A.1 for a description) The isochrones are in the tar gzipped file isoc_revagb.tar.gz that contains: ./isocz004al168.dat -> isochrones for Z=0.004, and alpha_MLT=1.68 ./isocz004al200.dat -> isochrones for Z=0.004, and alpha_MLT=2.00 ./isocz004al250.dat -> isochrones for Z=0.004, and alpha_MLT=2.50 ./isocz008al168.dat -> isochrones for Z=0.008, and alpha_MLT=1.68 ./isocz008al200.dat -> isochrones for Z=0.008, and alpha_MLT=2.00 ./isocz008al250.dat -> isochrones for Z=0.008, and alpha_MLT=2.50 ./isocz019al168.dat -> isochrones for Z=0.019, and alpha_MLT=1.68 ./isocz019al200.dat -> isochrones for Z=0.019, and alpha_MLT=2.00 ./isocz019al250.dat -> isochrones for Z=0.019, and alpha_MLT=2.50 They differ from Girardi et al. (2000) isochrones (see http://pleiadi.oapd.inaf.it/index.html#data4 ) in the region corresponding to TP-AGB stars. Isochrones with alpha_MLT=1.68 are perfectly homogeneous and continuous. Those with alpha_MLT=2.00 and alpha_MLT=2.50 have been computed with a higher mixing length parameter (and hence more efficient hot bottom burning) for TP-AGB stars of masses between 3.5 and 5.0 Msun. All details about the evolutionary tracks can be found in the papers Marigo (2001), A&A 370, 194; Girardi et al. (2000), A&AS 141, 371; Marigo et al. (1999), A&A 344, 123; Marigo (1998), A&A 340, 463; Marigo et al. (1998), A&A 331, 564. Each file contains a complete series of isochrones with log(age/yr) values going from 7.80 to 10.20 (i.e. from 0.063 to 15.8 Gyr), at equally spaced intervals of Delta(log age)=0.05 (i.e., two consecutive isochrones differ by only 12 percent in their ages.) FOR EACH ISOCHRONE, THE FOLLOWING INFORMATION IS PRESENTED: HEADER LINE: contains the exact age and metallicity value of the isochrone; Column (1) log(age/yr) --> logarithm of the age; Column (2) M_ini --> initial mass of the star; Column (3) M_act --> actual mass of the star, i.e., the mass obtained considering the previous history of mass-loss; Column (4) logL/Lo --> logarithm of surface luminosity (in solar units), log(L/Lsun); Column (5) logTef --> logarithm of effective temperature (in K), log(Teff/K); Column (6) logG --> logarithm of surface gravity (in cgs units); Column (7) Mbol --> absolute bolometric magnitude; Column (8) Mu --> absolute magnitude in the U pass-band; Column (9) Mb --> absolute magnitude in the B pass-band; Column (10) Mv --> absolute magnitude in the V pass-band; Column (11) Mr --> absolute magnitude in the R pass-band; Column (12) Mi --> absolute magnitude in the I pass-band; Column (13) Mj --> absolute magnitude in the J pass-band; Column (14) Mh --> absolute magnitude in the H pass-band; Column (15) Mk --> absolute magnitude in the K pass-band; Column (16) FLUM --> indefinite integral of the Salpeter IMF by number (see Girardi et al. 2000 for more details); ******************************************************** TABLES OF STELLAR FUELS (TABLES A.1 - A.3) The file tabfuel.tar.gz contains tables of post-MS stellar fuels for all evolutionary tracks of low- and intermediate-mass stars. They are described in Appendix A.2: ./fuelz019.dat -> Table A.1 ./fuelz008.dat -> Table A.2 ./fuelz004.dat -> Table A.3 To the tables, we have also appended models with 3.5 - 5.0 Msun computed with a mixing length parameter, alphaML, that is different from the usual one (1.68) during the TP-AGB phase. The last column specifies the value of alphaML that corresponds to the F_(TP-AGB) value in each line.