English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT
Add to Basket
  Local TagsRelease HistoryDetailsSummary

Released
Journal Article

Signatures of the many supermassive black hole mergers in a cosmologically forming massive early-type galaxy

MPS-Authors
/persons/resource/persons247771

Rantala,  Antti
Galaxy Formation, Cosmology, MPI for Astrophysics, Max Planck Society;

/persons/resource/persons16252

Naab,  Thorsten
Computational Structure Formation, MPI for Astrophysics, Max Planck Society;

External Resource
No external resources are shared
Fulltext (restricted access)
There are currently no full texts shared for your IP range.
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available
Citation

Mannerkoski, M., Johansson, P. H., Rantala, A., Naab, T., Liao, S., & Rawlings, A. (2022). Signatures of the many supermassive black hole mergers in a cosmologically forming massive early-type galaxy. The Astrophysical Journal, 929(2): 167. doi:10.3847/1538-4357/ac5f0b.


Cite as: https://hdl.handle.net/21.11116/0000-000B-54E1-8
Abstract
We model here the merger histories of the supermassive black hole (SMBH) population in the late stages of a cosmological simulation of a ∼ 2 × 1013M⊙ galaxy group. The gravitational dynamics around the several tens of SMBHs (M• > 7.5 × 107M⊙) hosted by the galaxies in the group is computed at high accuracy using regularized integration with the KETJU code. The 11 SMBHs that form binaries and a hierarchical triplet eventually merge after hardening through dynamical friction, stellar scattering, and gravitational wave (GW) emission. The binaries form at eccentricities of e ∼ 0.3–0.9, with one system evolving to a very high eccentricity of e = 0.998, and merge on timescales of a few tens to several hundred megayears. During the simulation, the merger-induced GW recoil kicks eject one SMBH remnant from the central host galaxy. This temporarily drives the galaxy off the M•–σ⋆ relation; however, the galaxy returns to the relation due to subsequent galaxy mergers, which bring in new SMBHs. This showcases a possible mechanism contributing to the observed scatter of the M•–σ⋆ relation. Finally, we show that pulsar timing arrays and LISA would be able to detect parts of the GW signals from the SMBH mergers that occur during the ∼4 Gyr time span simulated with KETJU.