Simulated data used for the analysis presented in the paper by Chruslinska, M., Nelemans, G., MNRAS, 2019. (DOI: 10.1093/mnras/stz2057).
The values in each file correspond to stellar mass density (comoving; Msun/Mpc^3) formed in a given 12+log(O/H) (columns) bin and between two redshifts (rows). The attached python script plot_SFRD_Z_z.py can be used to visualize the data.

File names: XYZfn_FOH_z_dM.dat 
where X,Y and Z specify the model variation.

X specifies the choice of the high mass part of the SFMR:
    X=1 : moderate flattening
    X=2 : sharp flattening
    X=3 : no flattening

Y specifies choice of the low mass end of the GSMF:
    Y=0 : alpha_fix = -1.45
    Y=1 : alpha_fix = alpha_fix(z)

Z specifies the choice of the MZR:
    Z=1 : T04 
    Z=2 : KK04
    Z=3 : M09
    Z=4 : PP04

n gives the value of $\sigma_{\nabla O/H}$ (scatter in metallicity within galaxies) used in the calculations:
    n=14 -> $\sigma_{\nabla O/H}$=0.14 (default choice)
    n=1  -> $\sigma_{\nabla O/H}$=0.1
    n=2  -> $\sigma_{\nabla O/H}$=0.2

e.g. 302f14_FOH_z_dM.dat is the data file corresponding to the high-Z extreme, 204f14_z_dM.dat to the low-Z extreme and 103f14_FOH_z_dM.dat to the moderate variation from the paper.
