Contribution of stripped nuclear clusters to globular cluster and ultracompact dwarf galaxy populations

Pfeffer, J., Griffen, B. F., Baumgardt, H. and Hilker, M. (2014) Contribution of stripped nuclear clusters to globular cluster and ultracompact dwarf galaxy populations. Monthly Notices of the Royal Astronomical Society, 444 4: 3670-3683. doi:10.1093/mnras/stu1705


Author Pfeffer, J.
Griffen, B. F.
Baumgardt, H.
Hilker, M.
Title Contribution of stripped nuclear clusters to globular cluster and ultracompact dwarf galaxy populations
Journal name Monthly Notices of the Royal Astronomical Society   Check publisher's open access policy
ISSN 0035-8711
1365-2966
Publication date 2014-11
Year available 2014
Sub-type Article (original research)
DOI 10.1093/mnras/stu1705
Open Access Status DOI
Volume 444
Issue 4
Start page 3670
End page 3683
Total pages 14
Place of publication Oxford, United Kingdom
Publisher Oxford University Press
Collection year 2015
Language eng
Formatted abstract
We use the Millennium II cosmological simulation combined with the semi-analytic galaxy formation model of Guo et al. to predict the contribution of galactic nuclei formed by the tidal stripping of nucleated dwarf galaxies to globular cluster (GC) and ultracompact dwarf galaxy (UCD) populations of galaxies. We follow the merger trees of galaxies in clusters back in time and determine the absolute number and stellar masses of disrupted galaxies. We assume that at all times nuclei have a distribution in nucleus-to-galaxy mass and nucleation fraction of galaxies similar to that observed in the present day Universe. Our results show stripped nuclei follow a mass function N(M) ∼ M−1.5 in the mass range 106 < M/M⊙ < 108, significantly flatter than found for globular clusters. The contribution of stripped nuclei will therefore be most important among high-mass GCs and UCDs. For the Milky Way we predict between one and three star clusters more massive than 105 M come from tidally disrupted dwarf galaxies, with the most massive cluster formed having a typical mass of a few times 106 M, like ω Centauri. For a galaxy cluster with a mass 7 × 1013 M, similar to Fornax, we predict ∼19 UCDs more massive than 2 × 106 M and ∼9 UCDs more massive than 107 M within a projected distance of 300 kpc come from tidally stripped dwarf galaxies. The observed number of UCDs are ∼200 and 23, respectively. We conclude that most UCDs in galaxy clusters are probably simply the high-mass end of the GC mass function.
Keyword Methods numerical
Galaxies dwarf
Galaxies formation
Galaxies interactions
Galaxies star clusters general
Ultra Compact Dwarf
Massive star clusters
Q-Index Code C1
Q-Index Status Confirmed Code
Institutional Status UQ

Document type: Journal Article
Sub-type: Article (original research)
Collections: School of Mathematics and Physics
Official 2015 Collection
 
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Citation counts: TR Web of Science Citation Count  Cited 14 times in Thomson Reuters Web of Science Article | Citations
Scopus Citation Count Cited 16 times in Scopus Article | Citations
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