2020ApJ...901...74T

We present 0.''2 resolution Atacama Large Millimeter/submillimeter Array (ALMA) observations at 870 µm in a stellar mass-selected sample of 85 massive (M_*> 10¹¹M_☉) star-forming galaxies (SFGs) at z=1.9–2.6 in the CANDELS/3D-Hubble Space Telescope fields of UDS and GOODS-S. We measure the effective radius of the rest-frame far-infrared (FIR) emission for 62 massive SFGs. They are distributed over wide ranges of FIR size from R_e,FIR=0.4kpc to R_e,FIR=6kpc. The effective radius of the FIR emission is smaller by a factor of 2.3_–1.0^+1.9 than the effective radius of the optical emission and is smaller by a factor of 1.9_–1.0^+1.9 than the half-mass radius. Taking into account potential extended components, the FIR size would change only by ∼10%. By combining the spatial distributions of the FIR and optical emission, we investigate how galaxies change the effective radius of the optical emission and the stellar mass within a radius of 1 kpc, M_1kpc. The compact starburst puts most of the massive SFGs on the mass-size relation for quiescent galaxies (QGs) at z ∼ 2 within 300 Myr if the current star formation activity and its spatial distribution are maintained. We also find that within 300 Myr, ∼38% of massive SFGs can reach the central mass of M_1kpc=10^10.5M_☉, which is around the boundary between massive SFGs and QGs. These results suggest an outside-in transformation scenario in which a dense core is formed at the center of a more extended disk, likely via dissipative in-disk inflows. Synchronized observations at ALMA 870 µm and James Webb Space Telescope 3-4 µm will explicitly verify this scenario.