Yu-Hsiu Huang (ASIAA/NTU); Hiroyuki Hirashita (ASIAA)
Interstellar dust plays an important role in radiative processes and star formation in galaxies. These processes are highly affected by the dust properties such as grain size distribution. On the other hand, the evolution of dust is related to the physical conditions and the galaxy assembly history. To understand the complicated processes of dust evolution, we implement our dust model in the state-of-art cosmological simulation IllustrisTNG (TNG). In previous work, we focused on Milky Way-like (MW-like) galaxies and successfully reproduced the Milky Way extinction curve. As for this work, we go further into higher redshift and target star-forming galaxies at $z=2$ in TNG. At $z=2$, the grain size distribution of our new sample is dominated by large grains and the dispersion in the large grain regime is small, which is different from the dust size evolution of the MW-like galaxies. For more robust comparison with observed properties of star-forming galaxies at the cosmic noon, we apply radiative transfer code SKIRT and calculate the spectral energy distribution for each galaxies. In particular, we discuss the attenuation curves and the IRX-$\beta$ relation predicted by our models.