STELLAR POPULATIONS ACROSS THE BLACK HOLE MASS-VELOCITY DISPERSION RELATION

• Published in: Astrophysical journal. Letters Vol. 832; no. 1; p. L11
• Main Authors: Martín-Navarro, Ignacio, Brodie, Jean P., van den Bosch, Remco C. E., Romanowsky, Aaron J., Forbes, Duncan A.
• Format: Journal Article
• Language: English
• Published: United States The American Astronomical Society 20.11.2016
• Subjects: Active galactic nuclei; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BLACK HOLES; Black holes (astronomy); DISPERSION RELATIONS; DISPERSIONS; EVOLUTION; FEEDBACK; GALAXIES; galaxies: active; galaxies: evolution; galaxies: formation; galaxies: fundamental parameters; galaxies: general; galaxies: stellar content; Galaxy formation; GALAXY NUCLEI; Local group (astronomy); MASS; SIMULATION; Star formation; STARS; Stellar populations; UNIVERSE; VELOCITY
• ISSN: 2041-8205; 2041-8213
• DOI: 10.3847/2041-8205/832/1/L11

ABSTRACT Coevolution between supermassive black holes (BH) and their host galaxies is universally adopted in models for galaxy formation. In the absence of feedback from active galactic nuclei (AGNs), 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- relation as a working framework. We find that over-massive BH galaxies, i.e., galaxies lying above the best-fitting BH mass- line, tend to be older and more -element-enhanced than under-massive BH galaxies. The scatter in the BH mass- -[ /Fe] plane is significantly lower than that in the standard BH mass- relation. We interpret this trend as an imprint of AGN feedback on the star formation histories of massive galaxies.