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MOCCA-survey data base: extra galactic globular clusters – II. Milky Way and Andromeda

Leveque, A. ; Giersz, M. ; Arca-sedda, M and Askar, Abbas LU orcid (2022) In Monthly Notices of the Royal Astronomical Society 514(4). p.5751-5766
Abstract
A comprehensive study of the co-evolution of globular cluster systems (GCS) in galaxies requires the ability to model both the large-scale dynamics (0.01–10 kpc) regulating their orbital evolution, and the small-scale dynamics (sub-pc – au) regulating the internal dynamics of each globular cluster (GC). In this work, we present a novel method that combine semi-analytic models of GCS with fully self-consistent Monte Carlo models to simultaneously evolve large GCSs. We use the population synthesis code MASinGa and the MOCCA-Survey Database I to create synthetic GC populations aimed at representing the observed features of GCs in the Milky Way (MW) and Andromeda (M31). Our procedure enables us to recover the spatial and mass distribution of... (More)
A comprehensive study of the co-evolution of globular cluster systems (GCS) in galaxies requires the ability to model both the large-scale dynamics (0.01–10 kpc) regulating their orbital evolution, and the small-scale dynamics (sub-pc – au) regulating the internal dynamics of each globular cluster (GC). In this work, we present a novel method that combine semi-analytic models of GCS with fully self-consistent Monte Carlo models to simultaneously evolve large GCSs. We use the population synthesis code MASinGa and the MOCCA-Survey Database I to create synthetic GC populations aimed at representing the observed features of GCs in the Milky Way (MW) and Andromeda (M31). Our procedure enables us to recover the spatial and mass distribution of GCs in such galaxies, and to constrain the amount of mass that GCs left either in the halo as dispersed debris, or in the galactic centre, where they can contribute to the formation of a nuclear star cluster (NSC) and can bring stellar and possibly intermediate mass black holes there. The final masses reported by our simulations are of a few order of magnitudes smaller than the observed values. These differences show that mass build-up of an NSC and central BHs in galaxies like MW and M31 cannot be solely explained by the infalling GC scenario. This build-up is likely to depend on the interplay between interactions and mergers of infalling GCs and gas. The latter can contribute to both in situ star formation in the NSC and growth of the central BH. (Less)
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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
514
issue
4
pages
16 pages
publisher
Oxford University Press
external identifiers
  • scopus:85135192525
ISSN
1365-2966
DOI
10.1093/mnras/stac1694
language
English
LU publication?
yes
id
f7409e9a-a43c-4879-a8f5-cd5924868753
date added to LUP
2022-07-18 14:19:14
date last changed
2024-04-18 12:55:00
@article{f7409e9a-a43c-4879-a8f5-cd5924868753,
  abstract     = {{A comprehensive study of the co-evolution of globular cluster systems (GCS) in galaxies requires the ability to model both the large-scale dynamics (0.01–10 kpc) regulating their orbital evolution, and the small-scale dynamics (sub-pc – au) regulating the internal dynamics of each globular cluster (GC). In this work, we present a novel method that combine semi-analytic models of GCS with fully self-consistent Monte Carlo models to simultaneously evolve large GCSs. We use the population synthesis code MASinGa and the MOCCA-Survey Database I to create synthetic GC populations aimed at representing the observed features of GCs in the Milky Way (MW) and Andromeda (M31). Our procedure enables us to recover the spatial and mass distribution of GCs in such galaxies, and to constrain the amount of mass that GCs left either in the halo as dispersed debris, or in the galactic centre, where they can contribute to the formation of a nuclear star cluster (NSC) and can bring stellar and possibly intermediate mass black holes there. The final masses reported by our simulations are of a few order of magnitudes smaller than the observed values. These differences show that mass build-up of an NSC and central BHs in galaxies like MW and M31 cannot be solely explained by the infalling GC scenario. This build-up is likely to depend on the interplay between interactions and mergers of infalling GCs and gas. The latter can contribute to both in situ star formation in the NSC and growth of the central BH.}},
  author       = {{Leveque, A. and Giersz, M. and Arca-sedda, M and Askar, Abbas}},
  issn         = {{1365-2966}},
  keywords     = {{galaxies: star clusters: general}},
  language     = {{eng}},
  month        = {{07}},
  number       = {{4}},
  pages        = {{5751--5766}},
  publisher    = {{Oxford University Press}},
  series       = {{Monthly Notices of the Royal Astronomical Society}},
  title        = {{MOCCA-survey data base: extra galactic globular clusters – II. Milky Way and Andromeda}},
  url          = {{http://dx.doi.org/10.1093/mnras/stac1694}},
  doi          = {{10.1093/mnras/stac1694}},
  volume       = {{514}},
  year         = {{2022}},
}