Hostname: page-component-78c5997874-94fs2 Total loading time: 0 Render date: 2024-11-10T17:15:05.819Z Has data issue: false hasContentIssue false
  • English
  • Français

Substructure in black hole scaling diagrams and implications for the coevolution of black holes and galaxies

Published online by Cambridge University Press:  29 March 2021

Benjamin L. Davis Open the ORCID record for Benjamin L. Davis [Opens in a new window] ,
Nandini Sahu  and
Alister W. Graham
Benjamin L. Davis
Affiliation:
Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia emails: benjamindavis@swin.edu.au, nsahu@swin.edu.au, agraham@swin.edu.au
Nandini Sahu
Affiliation:
Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia emails: benjamindavis@swin.edu.au, nsahu@swin.edu.au, agraham@swin.edu.au
Alister W. Graham
Affiliation:
Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia emails: benjamindavis@swin.edu.au, nsahu@swin.edu.au, agraham@swin.edu.au
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Our multi-component photometric decomposition of the largest galaxy sample to date with dynamically-measured black hole masses nearly doubles the number of such galaxies. We have discovered substantially modified scaling relations between the black hole mass and the host galaxy properties, including the spheroid (bulge) stellar mass, the total galaxy stellar mass, and the central stellar velocity dispersion. These refinements partly arose because we were able to explore the scaling relations for various sub-populations of galaxies built by different physical processes, as traced by the presence of a disk, early-type versus late-type galaxies, or a Sérsic versus core-Sérsic spheroid light profile. The new relations appear fundamentally linked with the evolutionary paths followed by galaxies, and they have ramifications for simulations and formation theories involving both quenching and accretion.

Keywords

black hole physicsgalaxies: bulgesgalaxies: elliptical and lenticular, cDgalaxies: evolutiongalaxies: kinematics and dynamicsgalaxies: spiralgalaxies: structure
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S359: Galaxy Evolution and Feedback across Different Environments , March 2019 , pp. 37 - 39
Copyright
© The Author(s), 2021. Published by Cambridge University Press on behalf of International Astronomical Union

References

Ciambur, B. C. 2015, ApJ, 810, 120 CrossRefGoogle Scholar
Ciambur, B. C. 2016, PASA, 33, e062 CrossRefGoogle Scholar
Davis, B. L., Graham, A. W., & Cameron, E. 2018, ApJ, 869, 113 CrossRefGoogle Scholar
Davis, B. L., Graham, A. W., & Cameron, E. 2019, ApJ, 873, 85 10.3847/1538-4357/aaf3b8CrossRefGoogle Scholar
Sahu, N., Graham, A. W., & Davis, B. L. 2019a, ApJ, 876, 155 10.3847/1538-4357/ab0f32CrossRefGoogle Scholar
Sahu, N., Graham, A. W., & Davis, B. L. 2019b, ApJ, 887, 10 CrossRefGoogle Scholar