  Recent cosmological hydrodynamical simulations have produced populations of
numerical galaxies whose global star-forming properties are in good agreement
with those of observed galaxies. Proper modeling of energetic feedback from
supernovae and active galactic nuclei is critical to the ability of simulations
to reproduce observed galaxy properties and, historically, such modelling has
proven to be a challenge. Here, we analyze local properties of central and
satellite galaxies in the $z=0$ snapshot of the TNG100 simulation as a test of
feedback models. We generate a face-on projection of stellar particles in
TNG100 galaxies, from which we demonstrate the existence of a resolved
star-forming main sequence ($\Sigma_{SFR}$--$\Sigma_*$ relation) with a slope
and normalization that is in reasonable agreement with previous studies. We
also present radial profiles of various galaxy populations for two parameters:
the distance from the resolved main sequence line ($\Delta\Sigma_{SFR}$) and
the luminosity-weighted stellar age ($age_L$). We find that, on average,
high-mass central and satellite galaxies quench from the inside-out, while
low-mass central and satellite galaxies have similar, flatter profiles.
