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 \sim 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 \sim - 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 .