an isolated Milky-Way-like galaxy by post-processing a hydrodynamic simulation. They put particular focus on the effect of gas-temperature-dependent sticking coefficient on dust growth by accretion, in order to reproduce the relation between silicon depletion and gas density. [@2019MNRAS.487.3252H] simulated the dust evolution in the ISM, focusing on dust destruction by sputtering. Although they did not trace the entire galaxy, their focus on a small region in the ISM enabled them to resolve the structures associated with SN shocks. We also note that there are some non-hydrodynamic approaches using semi-analytic models that predicted the evolution of dust mass in galaxies [@2017MNRAS.471.3152P; @2014MNRAS.445.3039D; @2018MNRAS.473.4538G; @2019MNRAS.489.4072V].

@2017MNRAS.466..105A [hereafter A17] implemented a two-size grain model in the cosmological smoothed particle hydrodynamics (SPH) code <span style="font-variant:small-caps;">gadget3-osaka</span> (A17; @2019MNRAS.484.2632S), which is a modified version of <span style="font-variant:small-caps;">gadget-3</span> [originally described in @2005MNRAS.364.1105S as <span style="font-variant:small-caps;">gadget-2</span>]. Their treatment of dust is based on the *two-size approximation* [@2015MNRAS.447.2937H], in which the entire grain radius range is divided into ‘large’ and ‘small’ grains. The two-size approximation reduces the computational cost in calculating the evolution of grain size distribution, so that it is easily implemented in hydrodynamic simulations. A17 performed simulations of a Milky-Way-like isolated galaxy, and explained the radial distribution 