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Stellar Populations across the Black Hole Mass–Velocity Dispersion Relation
The Astrophysical Journal Letters (2016)
  • Ignacio Martín-Navarro, University of California Observatories
  • Jean P. Brodie, University of California Observatories
  • Remco C.E. van den Bosch, Max Planck Institute for Astronomy
  • Aaron J. Romanowsky, San Jose State University
  • Duncan A. Forbes, Swinburne University of Technology
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–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 that in the standard BH mass–σ relation. We interpret this trend as an imprint of AGN feedback on the star formation histories of massive galaxies.
  • galaxies: active,
  • galaxies: evolution,
  • galaxies: formation,
  • galaxies: fundamental parameters,
  • galaxies: general,
  • galaxies: stellar content
Publication Date
Publisher Statement
This article was originally published in The Astrophysical Journal Letters, volume 832, issue 1. © 2016. The American Astronomical Society. All rights reserved.

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Citation Information
Ignacio Martín-Navarro, Jean P. Brodie, Remco C.E. van den Bosch, Aaron J. Romanowsky, et al.. "Stellar Populations across the Black Hole Mass–Velocity Dispersion Relation" The Astrophysical Journal Letters Vol. 832 Iss. 1 (2016) ISSN: 2041-8205
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