M-σ relations across cosmic time

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 million to hundreds of millions of years, these cluster, merger-triggered jetted AGN, will evolve mostly 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.