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MOCCA-Survey Database: extra galactic globular clusters – III. The population of black holes in Milky Way and Andromeda-like galaxies

Leveque, A. ; Giersz, M. ; Askar, Abbas LU orcid ; Arca-Sedda, M. and Olejak, A. (2023) In Monthly Notices of the Royal Astronomical Society 520(2). p.2593-2610
Abstract
This work investigates the black hole (BH) population of globular
clusters (GCs) in Milky Way- and Andromeda-like galaxies. We combine the
population synthesis code MASinGa and the MOCCA-Survey Database I to
infer the properties of GCs harbouring a stellar-mass BH subsystem
(BHS), an intermediate-mass BH (IMBH), or neither of those. We find that
the typical number of GCs with a BHS, an IMBH, or none become
comparable in the galactic outskirts, whilst the inner galactic regions
are dominated by GCs without a significant dark component. We retrieve
the properties of binary BHs (BBHs) that have either merged in the last
3 Gyr or survived in their parent cluster until present-day. We find
that... (More)
This work investigates the black hole (BH) population of globular
clusters (GCs) in Milky Way- and Andromeda-like galaxies. We combine the
population synthesis code MASinGa and the MOCCA-Survey Database I to
infer the properties of GCs harbouring a stellar-mass BH subsystem
(BHS), an intermediate-mass BH (IMBH), or neither of those. We find that
the typical number of GCs with a BHS, an IMBH, or none become
comparable in the galactic outskirts, whilst the inner galactic regions
are dominated by GCs without a significant dark component. We retrieve
the properties of binary BHs (BBHs) that have either merged in the last
3 Gyr or survived in their parent cluster until present-day. We find
that around 80 per cent of the merging BBHs form due to dynamical
interactions while the remaining originate from evolution of primordial
binaries. The inferred merger rate for both in-cluster and ejected
mergers is 1.0−23yr−1Gpc−3
in the local Universe, depending on the adopted assumptions. We find
around 100–240 BBHs survive in GCs until present-day and are mostly
concentrated in the inner few kpc of the galaxy. When compared with the
field, GCs are at least two times more efficient in the formation of BHs
and binaries containing at least one BH. Around 1000–3000 single BHs
and 100–200 BBHs are transported into the galactic nucleus from
infalling clusters over a time span of 12 Gyr. We estimate that the
number of BHs and BBHs lurking in the star cluster to be about
1.4–2.2 × 104 and 700–1100, respectively. (Less)
Please use this url to cite or link to this publication:
author
; ; ; and
organization
publishing date
type
Contribution to journal
publication status
published
subject
keywords
galaxies: star clusters: general
in
Monthly Notices of the Royal Astronomical Society
volume
520
issue
2
pages
18 pages
publisher
Oxford University Press
external identifiers
  • scopus:85160206449
ISSN
1365-2966
DOI
10.1093/mnras/stad240
language
English
LU publication?
yes
id
8de99d7f-091b-4620-be6b-a38c6c4d2052
date added to LUP
2023-03-22 16:34:10
date last changed
2023-08-21 04:01:34
@article{8de99d7f-091b-4620-be6b-a38c6c4d2052,
  abstract     = {{This work investigates the black hole (BH) population of globular <br>
clusters (GCs) in Milky Way- and Andromeda-like galaxies. We combine the<br>
 population synthesis code MASinGa and the MOCCA-Survey Database I to <br>
infer the properties of GCs harbouring a stellar-mass BH subsystem <br>
(BHS), an intermediate-mass BH (IMBH), or neither of those. We find that<br>
 the typical number of GCs with a BHS, an IMBH, or none become <br>
comparable in the galactic outskirts, whilst the inner galactic regions <br>
are dominated by GCs without a significant dark component. We retrieve <br>
the properties of binary BHs (BBHs) that have either merged in the last <br>
3 Gyr or survived in their parent cluster until present-day. We find <br>
that around 80 per cent of the merging BBHs form due to dynamical <br>
interactions while the remaining originate from evolution of primordial <br>
binaries. The inferred merger rate for both in-cluster and ejected <br>
mergers is 1.0−23yr−1Gpc−3<br>
 in the local Universe, depending on the adopted assumptions. We find <br>
around 100–240 BBHs survive in GCs until present-day and are mostly <br>
concentrated in the inner few kpc of the galaxy. When compared with the <br>
field, GCs are at least two times more efficient in the formation of BHs<br>
 and binaries containing at least one BH. Around 1000–3000 single BHs <br>
and 100–200 BBHs are transported into the galactic nucleus from <br>
infalling clusters over a time span of 12 Gyr. We estimate that the <br>
number of BHs and BBHs lurking in the star cluster to be about <br>
1.4–2.2 × 10<sup>4</sup> and 700–1100, respectively.}},
  author       = {{Leveque, A. and Giersz, M. and Askar, Abbas and Arca-Sedda, M. and Olejak, A.}},
  issn         = {{1365-2966}},
  keywords     = {{galaxies: star clusters: general}},
  language     = {{eng}},
  month        = {{02}},
  number       = {{2}},
  pages        = {{2593--2610}},
  publisher    = {{Oxford University Press}},
  series       = {{Monthly Notices of the Royal Astronomical Society}},
  title        = {{MOCCA-Survey Database: extra galactic globular clusters – III. The population of black holes in Milky Way and Andromeda-like galaxies}},
  url          = {{http://dx.doi.org/10.1093/mnras/stad240}},
  doi          = {{10.1093/mnras/stad240}},
  volume       = {{520}},
  year         = {{2023}},
}