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We investigate how star formation quenching proceeds within central andsatellite galaxies using spatially resolved spectroscopy from the SDSS-IV MaNGADR15. We adopt a complete sample of star formation rate surface densities($\Sigma_{\rm SFR}$), derived in Bluck et al. (2020), to compute the distanceat which each spaxel resides from the resolved star forming main sequence($\Sigma_{\rm SFR} - \Sigma_*$ relation): $\Delta \Sigma_{\rm SFR}$. We studygalaxy radial profiles in $\Delta \Sigma_{\rm SFR}$, and luminosity weightedstellar age (${\rm Age_L}$), split by a variety of intrinsic and environmentalparameters. Via several statistical analyses, we establish that the quenchingof central galaxies is governed by intrinsic parameters, with central velocitydispersion ($\sigma_c$) being the most important single parameter. High masssatellites quench in a very similar manner to centrals. Conversely, low masssatellite quenching is governed primarily by environmental parameters, withlocal galaxy over-density ($\delta_5$) being the most important singleparameter. Utilising the empirical $M_{BH}$ - $\sigma_c$ relation, we estimatethat quenching via AGN feedback must occur at $M_{BH} \geq 10^{6.5-7.5}M_{\odot}$, and is marked by steeply rising $\Delta \Sigma_{\rm SFR}$ radialprofiles in the green valley, indicating `inside-out' quenching. On the otherhand, environmental quenching occurs at over-densities of 10 - 30 times theaverage galaxy density at z$\sim$0.1, and is marked by steeply declining$\Delta \Sigma_{\rm SFR}$ profiles, indicating `outside-in' quenching. Finally,through an analysis of stellar metallicities, we conclude that both intrinsicand environmental quenching must incorporate significant starvation of gassupply.

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