the same simulation setup but including a simple treatment for active galactic nucleus feedback, focused on the relations between dust-related quantities and galaxy characteristics. They broadly reproduced the statistical properties such as the dust mass function and the relation between dust-to-gas ratio and metallicity in the nearby Universe. They also investigated extinction curves. However, because these results are based on the two-size approximation, the accuracy of extinction curve is limited. [There is another approach for the evolution of grain size distribution based on the method of moments formulated by [@MATTSSON2016107]. This method is powerful in calculating the processes related to the moments of grain size distribution such as the total grain surface area. However, it is still difficult to calculate the extinction curves. An explicit solution for the full grain size distribution enables us to directly calculate the extinction curves as well as other quantities (e.g. the surface area) that require grain size information. ]{}

Recently, there have been some efforts to directly solve the evolution of full grain size distribution in galaxy-scale hydrodynamic simulations. [@2018MNRAS.478.2851M] developed a computational code that solves the evolution of full grain size distribution in an adaptive mesh hydrodynamic simulation code, [AREPO]{} [@2010MNRAS.401..791S]. They showed 