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The tight correlation between total galaxy stellar mass and star formationrate (SFR) has become known as the star forming main sequence. Using ~487,000spaxels from galaxies observed as part of the Sloan Digital Sky Survey MappingGalaxies at Apache Point Observatory (MaNGA) survey, we confirm previousresults that a correlation also exists between the surface densities of starformation (Sigma_SFR) and stellar mass (Sigma_mass) on kpc scales, representinga `resolved' main sequence. Using a new metric (Delta Sigma_SFR), whichmeasures the relative enhancement or deficit of star formation on aspaxel-by-spaxel basis relative to the resolved main sequence, we investigatethe SFR profiles of 864 galaxies as a function of their position relative tothe global star forming main sequence (Delta SFR). For galaxies above theglobal main sequence (positive Delta SFR) Delta Sigma_SFR is elevatedthroughout the galaxy, but the greatest enhancement in star formation occurs atsmall radii (< 3 kpc, or 0.5 R_e). Moreover, galaxies that are at least afactor of three above the main sequence show diluted gas phase metallicitiesout to 2 R_e, indicative of metal-poor gas inflows accompanying the starbursts.For quiescent/passive galaxies that lie at least a factor of 10 below the starforming main sequence there is an analogous deficit of star formationthroughout the galaxy with the lowest values of Delta Sigma_SFR in the central3 kpc. Our results are in qualitative agreement with the `compaction' scenarioin which a central starburst leads to mass growth in the bulge and mayultimately precede galactic quenching from the inside-out.

Star formation is boosted (and quenched) from the inside out: radial star formation profiles from MaNGA