  We exploit a sample of 80,000 SDSS central galaxies to investigate the effect
of AGN feedback on their evolution. We trace the demographics of
optically-selected AGN (Seyferts) as a function of their internal properties
and environment. We find that the preeminence of AGN as the dominant ionising
mechanism increases with stellar mass, overtaking star-formation for galaxies
with $M_\text{stellar} \geq 10^{11}M_\odot$. The AGN fraction changes
systematically with the galaxies' star-formation activity. Within the blue
cloud, this fraction increases as star-formation activity declines, reaching a
maximum near the green valley ($\sim 17 \pm 4\%$), followed by a decrease as
the galaxies transition into the red sequence. This systematic trend provides
evidence that AGN feedback plays a key role in regulating and suppressing star
formation. In general, Seyfert central galaxies achieve an early-type
morphology while they still host residual star formation. This suggests that,
in all environments, the morphology of Seyfert galaxies evolves from late- to
early-type before their star formation is fully quenched. Stellar mass plays an
important role in this morphological transformation: while low mass systems
tend to emerge from the green valley with an elliptical morphology (T-Type
$\sim -2.5 \pm 0.7$), their high-mass counterparts maintain a spiral morphology
deeper into the red sequence. In high-stellar-mass centrals, the fraction of
Seyferts increases from early- to late-type galaxies, indicating that AGN
feedback may be linked with the morphology and its transformation. Our analysis
further suggests that AGN are fuelled by their own host halo gas reservoir, but
when in group centrals can also increase their gas reservoir via interactions
with satellite galaxies.
