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tokens: (2009) applied an early version of the IGIMF theory where the IMF variation of individual star clusters was not applied. The modern IGIMF prescription used here with a possible top-heavy gwIMF further increases the resulting [Mg/Fe] value. 7. Conclusions This contribution publishes an open source galaxy evolution code that is able to vary the gwIMF according to the IGIMF theory (or any other variable IMF theory) at each time step, yielding the mass composition, supernova rate, and chemical composition evolution of the galaxy. Following Yan et al. (2017) and Jeřábková et al. (2018) , where the gwIMF for a single star formation epoch is derived according to the IGIMF theory, the newly developed code published here enables us, for the first time, to perform a comprehensive and detailed examination of the effect of applying a different IMF theory in the context of galaxy chemical evolution assuming an identical SFH. Our preliminary result of a high-mass starburst galaxy assuming different IMFs and the same SFH is shown in Sect. 6 ; the result assuming the same gwIMF (the IGIMF theory) but different SFHs is shown in Appendix A . A systematically varying gwIMF leads to a strong modification of the element composition of a galaxy (naturally reproducing the observed higher metallicity and α -enhancement of the massive elliptical galaxies), while the difference in SFH and recent star formation activity influences the interpreted property of a galaxy due to a difference in the luminosity-weighted observation. The star formation environment of massive ellipticals in the early Universe is very different from the local Universe where we calibrate the IGIMF theory. There is no guarantee that such an extrapolation of the theory would work, but it is certainly an inspiring step. We will use this open source code for more comprehensive and detailed studies for galaxies with different masses and SFHs and also develop a spatially resolved IGIMF formulation. Appendix A: Results for a log-normal SFH Fig. A.1. Same as Fig. 5 , but for the log-normal SFH shown in Fig. 2 that extends for 13 Gyr. Fig. A.2. Same as Fig. 6 , but comparing different SFHs instead of different IMF assumptions. The orange lines apply the boxy SFH and the red lines apply the log-normal SFH, both shown in Fig. 2 . The same colour-coding is applied from Figs. A.2 – A.7 . The serrated shape is caused by the dying stars with a lifetime shorter than 10 Myr (see Sect. 6.2 ). We note that the orange lines are the same as the orange lines in Fig. 6 . This section compares the simulation results applying the IGIMF theory, but with the two different SFHs shown in Fig. 2 . The log-normal SFH forms the same stellar mass, but on a more extended timescale. The tail of the SFH with a low SFR leads to a stellar population that receives a contribution every δ t = 10 Myr from a top-light gwIMF, which does not exist in the box-shaped SFH model described in the main text. Thus, a more realistic and extended