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** TABLES OF ISOCHRONES WITH IMPROVED TP-AGB MODELS **
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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.
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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.pd.astro.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);
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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.