Structural evolution in massive galaxies at z~2

Abstract

We present 0.2arcsec-resolution Atacama Large Millimeter/submillimeter Array observations at 870 $\mu$m in a stellar mass-selected sample of 85 massive ($M_{\mathrm{star}}>10^{11}{M}_{\odot }$) star-forming galaxies (SFGs) at z=1.9-2.6 in the 3D-HST/CANDELS 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_{\mathrm{e},\mathrm{FIR}}=$0.4 kpc to $R_{\mathrm{e},\mathrm{FIR}}=$6 kpc. The effective radius of the FIR emission is smaller by a factor of 2.3${}_{-1.0}^{+1.9}$ than the effective radius of the optical emission and by a factor of 1.9${}_{-1.0}^{+1.9}$ smaller than the half-mass radius. Even with taking into account potential extended components, the FIR size would change 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 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 $M_{1kpc}=10^{10.5}{M}_{\odot }$, 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 $\mu$m and JWST 3-4 $\mu$m will explicitly verify this scenario.

25 pages, 15 figures, 3 tables, accepted for publication in ApJ

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