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