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

TL;DR

This study examines the evolution of the spatially resolved star formation main sequence in massive disc galaxies from redshift 1 to 0, revealing inside-out quenching and stellar mass buildup patterns.

Contribution

It introduces an empirical model for radial profiles of stellar mass, SFR, and sSFR, explaining the inside-out quenching process and evolution of the spatially resolved SFMS.

Findings

Linear spatially resolved SFMS at z~1 for galaxies on the global SFMS.

Flattening of the relation at high surface densities for below-main-sequence galaxies.

Radial sSFR profiles decrease faster in the center, supporting inside-out quenching.

Abstract

We investigate a relation between surface densities of star formation rate (SFR) and stellar mass ($M_{*}$) at a $\sim 1$ kpc scale namely spatially resolved star formation main sequence (SFMS) in massive ($\log(M_{*}/M_{\odot})>10.5$) 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 $M_{*}$. We find a linear spatially resolved SFMS in the $z\sim 1$ galaxies that lie on the global SFMS, while a 'flattening' at high $\Sigma_{*}$ 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 $\Sigma_{*}$ than that at high $\Sigma_{*}$. 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 $\Sigma_{*}(r)$, $\Sigma_{\rm SFR}(r)$ 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 $z\sim 0$.