Star formation quenching stages of active and non-active galaxies

The mechanisms that bring galaxies to strongly reduce their star formation activity (star-formation quenching) is still poorly understood. To better study galaxy evolution, we propose a classification based on the maps of the ionised hydrogen distribution, traced by kpc-resolved, equivalent width of H$α$ maps, and the nuclear activity of the galaxies using information from the BPT diagnostic diagrams. Using these tools, we group a sample of 238 galaxies from the CALIFA survey in six quenching stages (QS): objects dominated by recent star formation; systems that present a quiescent-nuclear-ring structure in their centre; galaxies that are centrally-quiescent; galaxies with no clear pattern in their ionisation gas distribution - mixed; systems that posses only a few star-forming regions - nearly-retired, or galaxies that are completely quiescent - fully-retired. Regarding their nuclear activity, we further divide the galaxies into two groups - active systems that host a weak or strong AGN in their centre, and non-active objects. Galaxies grouped into quenching stage classes occupy specific locations on the star-formation-rate versus stellar mass diagram. The "Blue cloud" is populated by the star-forming and the quiescent-nuclear-ring galaxies, the "Green valley" is populated by centrally-quiescent and mixed systems, "Red sequence" by the nearly- and fully-retired objects. Generally, galaxies that host a weak or strong AGN show properties, comparable to the non-active counterparts at the same quenching stages, except for the AGN-hosting star-forming systems. The degree of the star-formation quenching increases along the present emission-line pattern sequence from star-forming to fully-retired. The proposed emission-line classes reinforce the "inside-out" quenching scenario, which foresees that the suppression of the star-formation begins from the central regions of the galaxies.