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The relation between GC systems and SMBH in spiral galaxies: The link to the M• – M* correlation

Published online by Cambridge University Press:  09 June 2023

Rosa A. González-Lópezlira Open the ORCID record for Rosa A. González-Lópezlira [Opens in a new window]
Rosa A. González-Lópezlira*
Affiliation:
Instituto de Radioastronomia y Astrofisica, UNAM, Campus Morelia
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Abstract

We explore the relationship between globular cluster total number, NGC, and central black hole mass, M•, in spiral galaxies. Including cosmic scatter, log M• ∝ (1.64 ± 0.24) log NGC. Whereas in ellipticals the correlation is linear [log M• ∝ (1.02 ± 0.10) log NGC], and hence could be due to statistical convergence through mergers, this mechanism cannot explain the much steeper correlation in spirals. Additionally, we derive total stellar galaxy mass, M*, from its two-slope correlation with NGC (Hudson et al. 2014). In the M• versus M* parameter space, with M* derived from NGC, M• ∝ (1.48 ± 0.18) log M* for ellipticals, and M• ∝ (1.21 ± 0.16) log M* for spirals. The observed agreement between ellipticals and spirals may imply that black holes and galaxies co-evolve through “calm” accretion, AGN feedback and other secular processes.

Keywords

black hole physicsgalaxies: spiralgalaxies: formationgalaxies: evolutiongalaxies: star clusters: generalglobular clusters: general
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 17 , Symposium S373: Resolving the Rise and Fall of Star Formation in Galaxies (Aug 2022) , August 2021 , pp. 314 - 317
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Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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