Full chemo-evolutionary models are presented here for for 6 different SFR coefficients (1*0.0001/Myr; 5*0.0001/Myr; 10*0.0001/Myr; 20*0.0001/Myr; 50*0.0001/Myr; 100*0.0001/Myr), two types of IMFs (with slopes 0.35, 1.35 and 2.35) and 17 different ages ranging from 1 to 17 Gyr. The SFR is assumed to be proportional to the fractional gas mass by a coefficient expressed in units of 0.0001/Myr. This coefficient determines the timescale of star formation (see for details Vazdekis et al. 1996). For the solar neighborhood this coefficient is approximately 1.9. The IMF is constant and does not evolve with time. Time-dependent IMF models can be found in Vazdekis et al. 1996 and Vazdekis et al. 1997. The computations are performed on the basis of the Bertelli et al. 1994 (A&AS,141,371) isochrones and the stellar tracks of Pols et al. 1995 (MNRAS,274,964) for the very low MS stars, which were transformed to the observational plane according to almost fully empirical relations. See Vazdekis et al. 1996) for a full description of these models.
CHEMOEVOL_UNIMODAL and CHEMOEVOL_BIMODAL files include the model predictions computed on the basis of unimodal and bimodal IMFs, respectively. The information per columns is as follows:
co(1)= SFR
Coefficient (1,5,10,20,50 and 100*0.0001/Myr)
co(2)= IMF
Slope (0.35, 1.35, 2.35)
co(3)= Age
(1-17 Gyr)
co(4)=
Final Metallicity (Zend)
co(5)=
Average Metallicity (<Z>)
co(6) ='U-V'
co(7) ='B-V'
co(8) ='V-R'
co(9) ='V-I'
co(10)='V-J'
co(11)='V-K'
co(12)='CN1'
(magnitude)
co(13)='CN2'
(magnitude)
co(14)='Ca4227'
(Angstrom)
co(15)='G-band'
(Angstrom)
co(16)='Fe4383'
(Angstrom)
co(17)='Ca4455'
(Angstrom)
co(18)='Fe4531'
(Angstrom)
co(19)='Fe4668'
(Angstrom)
co(20)='Hbeta'
(Angstrom)
co(21)='Fe5015'
(Angstrom)
co(22)='Mg1'
(magnitude)
co(23)='Mg2'
(magnitude)
co(24)='Mgb'
(Angstrom)
co(25)='Fe5270'
(Angstrom)
co(26)='Fe5335'
(Angstrom)
co(27)='Fe5406'
(Angstrom)
co(28)='Fe5709'
(Angstrom)
co(29)='Fe5782'
(Angstrom)
co(30)='NaD'
(Angstrom)
co(31)='TiO1'
(magnitude)
co(32)='TiO2'
(magnitude)
co(33)='CaII1'
(Angstrom)
co(34)='CaII2'
(Angstrom)
co(35)='CaII3'
(Angstrom)
co(36)='MgII'
(Angstrom)
co(37)='(M/L)V'
(Mass-to-light ratio in the V-band)
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