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

Abstract

We investigate a relation between surface densities of star formation rate (SFR) and stellar mass ($M_{\ast }$) at a $\sim 1$ kpc scale namely spatially resolved star formation main sequence (SFMS) in massive ($\log (M_{\ast }/M_{\odot })>10.5$) 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 $z\sim 0$ galaxies is discussed in a companion paper. For $z\sim 1$ 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 $M_{\ast }$. We find a linear spatially resolved SFMS in the $z\sim 1$ galaxies that lie on the global SFMS, while a 'flattening' at high ${\Sigma }_{\ast }$ end is found in that relation for the galaxies that lie below the global SFMS. Comparison with the spatially resolved SFMS of the $z\sim 0$ galaxies shows smaller difference in the specific SFR (sSFR) at low ${\Sigma }_{\ast }$ than that at high ${\Sigma }_{\ast }$. 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 ${\Sigma }_{\ast }(r)$, ${\Sigma }_{\mathrm{SFR}}(r)$ 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 $z\sim 1$ and $z\sim 0$.

20 pages, 21 figures. Updated with some supporting appendixes. Accepted by MNRAS

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