Bridging between the integrated and resolved main sequence of star
  formation
  The position of galaxies on the stellar mass, star formation rate plane with
respect to the star-forming main sequence at each redshift is a convenient way
to infer where the galaxy is in its evolution compared to the rest of the
population. We use Hubble Space Telescope high resolution images in the GOODS-S
field from the CANDELS survey and fit multi wavelength lights in resolution
elements of galaxies with stellar population synthesis models. We then
construct resolved kpc-scale stellar mass, star formation rate surface density
curves for galaxies at z~1. Fitting these resolved main sequence curves with
Schechter functions, we parameterize and explain the multi-wavelength structure
of galaxies with three variables: phi*, alpha, and M*. For quenched galaxies
below the main sequence, we find an average high mass slope (alpha) of the
resolved main sequence curves to be ~ -0.4. The scatter of this slope is higher
among the lower mass star forming galaxies and those above the main sequence
compared to quenched galaxies, due to lack of an evolved bulge. Our findings
agree well with an inside-out quenching of star-formation. We find that the
knee of the Schechter fits (M*) for galaxies below the main sequence occurs at
lower stellar mass surface densities compared to star forming galaxies, which
hints at how far quenching has proceeded outwards.
