GCE Data Release

Jump to the data format!

The code is described in Kobayashi+2000. Overview can be found in my book chapter.
If you use any of the data below please e-mail me priori to the submission of your paper, and cite both of the code paper and the data paper(s).
E-mail me if you want other models in my publications.

K06 models: Salpeter IMF in Kobayashi+2006.
K11 models: Kroupa IMF, with AGB stars in Kobayashi+2011.

MW models: Ch SNIa only, s-process, ECSN, NSM and MRSN are included (not nu-winds) but not WR
- sz: solar neighbourhood
- hz: halo use only t<5Gyr (lines 500) as SFR gets too low and not many stars form afterwords
- hz*to03: halo with stronger outflow use only t<2Gyr (lines 200)
- wbz: bulge with SF truncated by galactic winds use only t<3Gyr (lines 300)
- bz: bulge with SF suppressed by outflow
- wtz: thick disk use only t<3Gyr (lines 300)
- See Table 4 and Figure 2 of the K20 paper for the details.

dSph models: Ch and sub-Ch SNIa (*x50* files also include Iax), s-process, ECSN, NSM and MRSN are included (not nu-winds)
- izF: Fornax, use only at t=<12 Gyr
- wzScl: Sculptor, use only at t=<9 Gyr
- wzSex: Sextans, use only at t=<7 Gyr
- izCs: Carina, use only at t=<12 Gyr
- dzUFD: ultra-faint dwarfs, use only at t=<10 Gyr
- See Table 2 and Figure 19 of the SNIa paper for the details.

M31 models
- izM31w1_3 : fiducial
- izM31w1_2 : weaker first SF, metalicity not reaching too high
- wzM31 : outer thick disk
- Cite my M31 paper if you use any of these data.

README

K20 data format (*_x.dat): Text file, containing the time evolution of elemental abundances (mass ratio relative to a unit mass of the system) normalized by the solar ratios, X/X_sun (not logarithmic) for all stable elements (excluding 43Tc and 61Pm which are radioactive)
```
column 1: time in Gyr
column 2: H/H_sun
column 3: He/He_sun
column 4: Li/Li_sun
....
column 27: Fe/Fe_sun
...
column 82: Bi/Bi_sun
column 83: Th/Th_sun
column 84: U/U_sun
```
The solar abundances are mainly the photospheric values from Asplund et al. (2009),
except for A(Li)sun = 3.26, A(O)sun = 8.76, A(Pb)sun = 2.04, A(Th)sun = 0.22, A(U)sun = -0.02.
Reference: Kobayashi, Karakas, Lugaro 2020 (K20)
K06/K11/K15 old format (*_x.dat): The same as above, but for the elements from H to Ge only
```
read{t 1  H 2 He 3 Li 4 Be 5 B 6 C 7 N 8 O 9 F 10 Ne 11 Na 12 Mg 13}
read{Al 14 Si 15 P  16 S  17 Cl 18 Ar 19 K 20 Ca 21 Sc 22 Ti 23}
read{V  24 Cr 25 Mn 26 Fe 27 Co 28 Ni 29 Cu 30 Zn 31 Ga 32 Ge 33}
```
The solar abundances are taken from Anders & Grevesse (1989).
The Salpeter IMF is adopted for K06, while Kroupa IMF is adopted for the rest.
The contributions from AGB stars are included from K11.
The neutrino process is included only in Kobayahsi, Izutani et al. 2011
The jet-like explosion effects are included only for K15.

Isotopic ratios (*_xx.dat): The same as above, but for isotopic ratios from H to Ge (mass ratios relative to a unit mass of the system) normalized by the solar ratios, X/X_sun (not logarithmic).

read{t 1  H1 2 H2 3 He3 4 He4 5 Li6 6 Li7 7 Be9 8 B10 9 B11 10}
read{C12 11 C13 12 N14 13 N15 14 O16 15 O17 16 O18 17 F19 18 Ne20 19 Ne21 20}
read{Ne22 21 Na23 22 Mg24 23 Mg25 24 Mg26 25 Al27 26 Si28 27 Si29 28 Si30 29}
read{P31 30 S32 31 S33 32 S34 33 S36 34 Cl35 35 Cl37 36 Ar36 37 Ar38 38}
read{Ar40 39 K39 40 K40 41 K41 42 Ca40 43 Ca42 44 Ca43 45 Ca44 46 Ca46 47}
read{Ca48 48 Sc45 49 Ti46 50 Ti47 51 Ti48 52 Ti49 53 Ti50 54 V50 55 V51 56}
read{Cr50 57 Cr52 58 Cr53 59 Cr54 60 Mn55 61 Fe54 62 Fe56 63 Fe57 64 Fe58 65}
read{Co59 66 Ni58 67 Ni60 68 Ni61 69 Ni62 70 Ni64 71 Cu63 72 Cu65 73 Zn64 74}
read{Zn66 75 Zn67 76 Zn68 77 Zn70 78 Ga69 79 Ga71 80 Ge70 81}

We currently release only those without s/r (which are used in Figure 31 of the paper); those with s/r also exist but are not published yet.

Other basic quantities of a sysmten with a unit mass (*0.dat):

column 1: time [Gyr]
column 2: SFR* [/Gyr]
column 4: inflow rate* [/Gyr]
column 5: outflow rate* [/Gyr]
column 6: gas fraction*
column 7: stellar fraction*
column 8: gas metallicity [M/H]
column 9: mean stellar metallicity <[M/H]>_*
column 10: gas-phase iron abundance [Fe/H]
column 11: mean stellar iron abundance <[Fe/H]>_*
column 12: gas-phase oxygen abundance [O/H]
column 13: mean stellar oxygen abundance <[O/H]>_* ~ <[Mg/H]>_*

* per unit solar mass of the system. In the models with no outflows/winds, the integral of inflow rate over t=0 to t=infinity is set to be 1.
See Kobayashi+2000 for the equations of SFR & inflow, and Kobayashi+2006 for outflow.

Metallicity distribution functions (*_n.dat):

column 1: [Fe/H] or [O/H] bin
column 2: raw number at [Fe/H] bin
column 3: observed number with 0.1 dex error
column 4: raw number at [O/H] bin
column 5: observed number with 0.1 dex error

Note that [O/H] = [O/Fe] + [Fe/H] ~ log Z/Zsun

Model parameters (*.par files): my long file names already contain most of the numbers. Below is the fiducial model for the solar neighborhood.

szzfc       ! name of model
1.3         ! index of initial mass function   -- x (kx denotes Kroupa)
1.0         ! index of star formation   -- ns
1.0         ! index of outflow    -- no
4.7         ! timescale of star formation (Gyr)   -- ts (1/ts gives the efficiency, as SFR is proportional to gas fraction)
5.0         ! timescale of inflow (Gyr)   -- ti
0.          ! timescale of outflow (Gyr)   -- to (ts/to gives the loading factor, as outflow rate is also proportional to gas fraction)
0.01        ! lower mass (Msun)
50.         ! upper mass (Msun)
3.0         ! lower mass of SNIa (Msun); for K06/K11 only, metallicity-dependent in K20
8.0         ! upper mass of SNIa (Msun); for K06/K11 only, metallicity-dependent in K20
0.9 1.8     ! lower mass of SNIa companion (Msun); for K06 only, metallicity-dependent in K11/K20
1.5 2.6     ! upper mass of SNIa companion (Msun); for K06 only, metallicity-dependent in K11/K20
0.02 0.04   ! SNIa parameters for RG+WD and MS+WD systems
0.0         ! initial gas mass   -- g (1.0 for a closed-box model)
0.01        ! time step (Gyr)
15.         ! end of time for calculation (Gyr)

See Kobayashi+2000 for the definitions of SFR & inflow parameters, and Kobayashi+2006 for outflow parameters.

Note again that abundance ratio in extra-galactic community is a number ratio not normalized by the solar ratio, but my data are mass ratios and are normalized, X/Xsun. Galactic users can just take the log of my table numbers to compare with observations [X/H], while extra-galactic users need the solar abundance table (e-mail me if you want the old version for K06/K11) and atomic mass. E.g., log N/O = log (X(N)/Xsun(N)/X(O)*Xsun(O)/14*16).
Usually the initial composition is set to be primordial, i.e., elements >= C is zero, using the Big Bang nuleosynthesis yields table (but with observed Li, see K20 paper). It is possible to run the code with any pre-enrichment if you want.

These data are owned and maintained by Chiaki Kobayashi (University of Hertfordshire), c.kobayashi at herts.ac.uk