How do central and satellite galaxies quench? - Insights from spatially resolved spectroscopy in the MaNGA survey

We investigate how star formation quenching proceeds within central and satellite galaxies using spatially resolved spectroscopy from the SDSS-IV MaNGA DR15. We adopt a complete sample of star formation rate surface densities (Delta Sigma(SFR)), derived in Bluck et al. (2020), to compute the distance at which each spaxel resides from the resolved star forming main sequence (Delta Sigma(SFR) - Sigma(*) relation): Delta Sigma(SFR). We study galaxy radial profiles in Delta Sigma(SFR), and luminosity weighted stellar age (Age(L)), split by a variety of intrinsic and environmental parameters. Via several statistical analyses, we establish that the quenching of central galaxies is governed by intrinsic parameters, with central velocity dispersion (sigma(c)) being the most important single parameter. High mass satellites quench in a very similar manner to centrals. Conversely, low mass satellite quenching is governed primarily by environmental parameters, with local galaxy overdensity (delta(5)) being the most important single parameter. Utilizing the empirical MBH - sigma(c) relation, we estimate that quenching via AGN feedback must occur at M-BH >= 10(6.5-7.5)M(circle dot), and is marked by steeply rising Delta Sigma(SFR) radial profiles in the green valley, indicating `inside-out' quenching. On the other hand, environmental quenching occurs at overdensities of 10-30 times the average galaxy density at z similar to 0.1, and is marked by steeply declining Delta Sigma(SFR) profiles, indicating `outside-in' quenching. Finally, through an analysis of stellar metallicities, we conclude that both intrinsic and environmental quenching must incorporate significant starvation of gas supply.