J/MNRAS/358/521 Grid of chemical evolution models for galaxies (Molla+, 2005)
A grid of chemical evolution models as a tool to interpret spiral and
irregular galaxies data.
Molla M., Diaz A.I.
<Mon. Not. R. Astron. Soc., 358, 521-543 (2005)>
=2005MNRAS.358..521M 2005MNRAS.358..521M
ADC_Keywords: Models, evolutionary ; Abundances
Keywords: galaxies: abundances - galaxies: evolution - galaxies: spirals -
galaxies: stellar content
Abstract:
We present a generalization of the multiphase chemical evolution model
applied to a wide set of theoretical galaxies with different masses
and evolutionary rates. This generalized set of models has been
computed using the so-called Universal Rotation Curve from Persic et
al. (1996MNRAS.281...27P 1996MNRAS.281...27P) to calculate the radial mass distribution of
44 theoretical protogalaxies. This distribution is a fundamental input
which, besides its own effect on the galaxy evolution, defines the
characteristic collapse time-scale or gas infall rate onto the disc.
We have adopted 10 sets of values, between 0 and 1, for the molecular
cloud and star formation efficiencies, as corresponding to their
probability nature, for each one of the radial distributions of total
mass. Thus, we have constructed a bi-parametric grid of models,
depending on those efficiency sets and on the rotation velocity, whose
results are valid in principle for any spiral or irregular galaxy. The
model results provide the time evolution of different regions of the
disc and the halo along galactocentric distance, measured by the gas
(atomic and molecular) and stellar masses, the star formation rate and
chemical abundances of 14 elements, for a total of 440 models. This
grid may be used to estimate the evolution of a given galaxy for which
only present time information, such as radial distributions of
elemental abundances, gas densities and/or star formation, which are
the usual observational constraints of chemical evolution models, is
available.
Description:
We show the chemical evolution model results for 440 theoretical
galaxies computed using the combination of 44 radial distribution of
total mass and 10 efficiencies set to form molecular clouds and stars
as possible inputs. Table 1 and Table 2 give these inputs while
table 3, table 4 and table 5 give the models results for the complete
grid. If you want only a model corresponding to a given total mass
radial distribution and/or a given efficiency set, go to models.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 50 44 Assumed galaxy characteristics dependent on the
total mass
table2.dat 19 10 Efficiencies of molecular cloud and star
formation processes
table3.dat 86 546630 Masses in each region and phase
table4.dat 76 546630 Star formation and SN rates in disk and halo
table5.dat 148 546630 Elemental abundances in mass
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See also:
J/A+A/432/861 : Low & intermediate mass stars yields (Gavilan+ 2005)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ndis Number of mass distribution in Table 1
5- 8 F4.2 2.5x10+10solLum lambda Galaxy-to-(Milky Way) luminosity ratio
(in units of 1010.4L☉)
12- 15 F4.1 kpc Ropt Optical radius
18- 22 F5.1 kpc Rgal Galaxy virial radius
25- 28 F4.1 kpc Rc Galaxy characteristic radius
31- 33 I3 km/s Vmax Rotation velocity
37- 41 I5 10+9solMass Mgal Galaxy total mass
45- 49 F5.2 Gyr tau Collapse time scale
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Nes Number of efficiencies set
4- 8 F5.3 --- emu Efficiency to form molecular clouds from
diffuse gas
11- 17 E7.2 --- eh Efficiency to form stars from molecular clouds
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ndis Number of mass distribution in Table 1
4- 5 I2 --- Nes Number of efficiencies set in Table 2
9- 12 F4.1 Gyr t Time of evolution
14- 15 I2 kpc R Galactocentric radius of each region
16 A1 --- --- [.]
18- 26 E9.2 10+9solMass Mtot Total Mass in the region
28- 36 E9.2 10+9solMass Mdisc Total Mass in the disk
38- 46 E9.2 10+9solMass MHI Total Mass in diffuse gas phase
48- 56 E9.2 10+9solMass MH2 Total Mass in molecular gas phase
58- 66 E9.2 10+9solMass Ms1 Total Mass in low mass stars (m<4Msun)
68- 76 E9.2 10+9solMass Ms2 Total Mass in massive stars (m>4Msun)
78- 86 E9.2 10+9solMass Mrmn Total Mass in remnants
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ndis Number of mass distribution in Table 1
4- 5 I2 --- Nes Number of efficiencies set in Table 2
9- 12 F4.1 Gyr t Time of evolution
14- 15 I2 kpc R Galactocentric radius of each region
16 A1 --- --- [.]
18- 26 E9.2 solMass/yr SFRdisc Star formation rate en the disk
28- 36 E9.2 solMass/yr SFRhalo Star formation rate in the halo
38- 46 E9.2 0.01/yr SNIad Supernova Ia rate in the disk
48- 56 E9.2 0.01/yr SNIId Supernova II rate in the disk
58- 66 E9.2 0.01/yr SNIah Supernova Ia rate in the halo
68- 76 E9.2 0.01/yr SNIIh Supernova II rate in the halo
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ndis Number of mass distribution in Table 1
4- 5 I2 --- Nes Number of efficiencies set in Table 2
9- 12 F4.1 Gyr t Time of evolution
14- 15 I2 kpc R Galactocentric radius of each region
16 A1 --- --- [.]
18- 22 F5.3 --- A(H) Hydrogen abundance by mass
24- 32 E9.2 --- A(D) Deuterium abundance by mass
34- 42 E9.2 --- A(3He) Helium-3 abundance by mass
44- 48 F5.3 --- A(4He) Helium-4 abundance by mass
50- 58 E9.2 --- A(12C) Carbon-12 abundance by mass
60- 68 E9.2 --- A(13C) Carbon-13 abundance by mass
70- 78 E9.2 --- A(N) Nitrogen abundance by mass
80- 88 E9.2 --- A(O) Oxygen abundance by mass
90- 98 E9.2 --- A(Ne) Neon abundance by mass
100-108 E9.2 --- A(Mg) Magnesium abundance by mass
110-118 E9.2 --- A(Si) Silicium abundance by mass
120-128 E9.2 --- A(S) Sulfur abundance by mass
130-138 E9.2 --- A(Ca) Calcium abundance by mass
140-148 E9.2 --- A(Fe) Iron abundance by mass
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Acknowledgements: Mercedes Molla, mercedes.molla(at)ciemat.es
(End) Patricia Vannier [CDS] 29-Mar-2005