# Spatial distribution of stellar mass and star formation activity at 0.2<z<1.2 across and along the Main Sequence

## TL;DR

This study uses high-resolution HST data to analyze the spatial distribution of star formation and stellar mass in galaxies across the Main Sequence at 0.2<z<1.2, revealing central star formation enhancement above the MS and suppression below it.

## Contribution

It provides spatially resolved maps of star formation and mass distribution in galaxies across the Main Sequence, highlighting inside-out quenching processes.

## Key findings

- Star formation is centrally enhanced above the MS and suppressed below it.
- Bulge growth occurs while galaxies are on the MS.
- Inside-out quenching is indicated by suppressed central star formation in below-MS galaxies.

## Abstract

High-resolution multi-wavelength photometry is crucial to explore the spatial distribution of star formation in galaxies and understand how these evolve. To this aim, in this paper we exploit the deep, multi-wavelength Hubble Space Telescope (HST) data available in the central parts of the GOODS fields and study the distribution of star formation activity and mass in galaxies located at different positions with respect to the Main Sequence (MS) of star-forming galaxies. Our sample consists of galaxies with stellar mass $\geq 10^{9.5} M_{\odot}$ in the redshift range 0.2 $ \leq z \leq 1.2$. Exploiting 10-band photometry from the UV to the near-infrared at HST resolution, we derive spatially resolved maps of galaxies properties, such as stellar mass and star formation rate and specific star formation rate, with a resolution of $\sim 0.16$ arcsec. We find that the star formation activity is centrally enhanced in galaxies above the MS and centrally suppressed below the MS, with quiescent galaxies (1 dex below the MS) characterised by the highest suppression. The sSFR in the outer region does not show systematic trends of enhancement or suppression above or below the MS. The distribution of mass in MS galaxies indicates that bulges are growing when galaxies are still on the MS relation. Galaxies below the MS are more bulge-dominated with respect to MS counterparts at fixed stellar mass, while galaxies in the upper envelope are more extended and have S\'ersic indexes that are always smaller than or comparable to their MS counterparts. The suppression of star formation activity in the central region of galaxies below the MS hints at \textit{inside-out} quenching, as star formation is still ongoing in the outer regions.