Stellar populations across the black hole mass - velocity dispersion relation

Abstract

Coevolution between supermassive black holes (BHs) and their host galaxies is universally adopted in models for galaxy formation. In the absence of feedback from active galactic nuclei, simulated massive galaxies keep forming stars in the local Universe. From an observational point of view, however, such coevolution remains unclear. We present a stellar population analysis of galaxies with direct BH mass measurements and the BH mass-σ relation as a working framework. We find that over-massive BH galaxies, i.e., galaxies lying above the best-fitting BH mass-σ line, tend to be older and more α-element enhanced than under-massive BH galaxies. The scatter in the BH mass-σ-[α/Fe] plane is significantly lower than in the standard BH mass-σ relation. We interpret this trend as an imprint of active galactic nucleus feedback on the star formation histories of massive galaxies.

6 pages, 4 figures, accepted for publication in ApJL

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• Anisotropic satellite galaxy quenching modulated by supermassive black hole activity
• Integral-field kinematics and stellar populations of early-type galaxies out to three half-light radii
• Gravitational Potential and Surface Density Drive Stellar Populations -- II. Star-Forming Galaxies
• The dark side of galaxy stellar populations I: The stellar-to-halo mass relation and the velocity dispersion - halo mass relation
• Star formation quenching imprinted on the internal structure of naked red nuggets
• Galaxies with monstrous black holes in galaxy cluster environments
• Quantifying the effect of black hole feedback from the central galaxy on the satellite populations of groups and clusters
• X-ray AGN in Boötes: The lack of growth of the most massive black holes since z=4