Evolution of spatially resolved star formation main sequence and surface density profiles in massive disc galaxies at 0 ≲ z ≲ 1: inside–out stellar mass buildup and quenching

We investigate a relation between surface densities of star formation rate (SFR) and stellar mass (M*) at a ~ 1 kpc scale namely spatially resolved star formation main sequence (SFMS) in massive (log(M*/M_)>10.5) face-on disc galaxies at $0.01<z<0.02$ and $0.8<z<1.8$ and examine evolution of the relation. The spatially resolved SFMS of z~ 0 galaxies is discussed in a companion paper. For z~ 1 sample, we use 8 bands imaging dataset from CANDELS and 3D-HST and perform a pixel-to-pixel SED fitting to derive the spatially resolved SFR and M*. We find a linear spatially resolved SFMS in the z~ 1 galaxies that lie on the global SFMS, while a 'flattening' at high Σ* end is found in that relation for the galaxies that lie below the global SFMS. Comparison with the spatially resolved SFMS of the z~ 0 galaxies shows smaller difference in the specific SFR (sSFR) at low Σ* than that at high Σ*. This trend is consistent with the evolution of the sSFR$(r)$ radial profile, which shows a faster decrease in the central region than in the outskirt, agrees with the inside-out quenching scenario. We then derive an empirical model for the evolution of the Σ*(r), ΣSFR(r) and sSFR$(r)$ radial profiles. Based on the empirical model, we estimate the radial profile of the quenching timescale and reproduce the observed spatially resolved SFMS at z~ 1 and z~ 0.