Feedback from active galactic nuclei (AGN) has long been invoked to explain
the correlation between black hole mass and stellar velocity dispersion
(M-
σ) discovered in low redshift galaxies. We describe the time
evolution of AGN in the M-
σ plane based on our gap model (Garofalo,
Evans \& Sambruna 2010) for black hole accretion and jet formation illustrating
a fundamental difference between jetted and non-jetted AGN. While the latter
tend to evolve diagonally upward with black hole mass increasing along with
stellar dispersion, we show that jetted AGN tend on average to move initially
more upwards because their effect on velocity dispersion is weaker than for
non-jetted AGN. But this initial phase is followed by a shift in the nature of
the feedback, from positive to negative, a transition that is more dramatic on
average in denser cluster environments. The feedback gets its kick from tilted
jets which shut down star formation but increase velocity dispersion values. As
this change in the nature of the feedback takes tens of millions to hundreds of
millions of years, these cluster, merger-triggered jetted AGN, will evolve more
upwards for up to order
108 years, followed by an extremely long phase in
which low excitation progressively slows black hole growth but dramatically
affects stellar dispersion. As a result, powerful jetted AGN evolve for most of
their lives almost horizontally on the M-
σ plane. The prediction is that
strongest AGN feedback on stellar dispersion is a late universe phenomenon with
M87 a good example. We show how jetted and non-jetted AGN parallel the Sersic
and core-Sersic galaxy paths in the M-
σ plane found by Sahu et al (2019)
and to a prediction that jetted quasars are not core-Sersic galaxies as found
for lower redshift jetted AGN.