期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 482, 期 4, 页码 4713-4725出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/sty1508
关键词
methods: numerical, stars: kinematics and dynamics, globular clusters: general, globular clusters: individual: omega; Centauri (NGC 5139), galaxies: star clusters: general
资金
- Royal Society
- ESA Research Fellowship
- European Research Council (CLUSTERS) [ERC StG-335936]
- NRC-Canada Plaskett Fellowship
- Radboud Excellence Initiative
The search for intermediate-mass black holes (IMBHs) in the centre of globular clusters is often based on the observation of a central cusp in the surface brightness profile and a rise towards the centre in the velocity dispersion profiles. Similar signatures, however, could result from other effects, that need to be taken into account in order to determine the presence (or the absence) of an IMBH in these stellar systems. Following our previous exploration of the role of radial anisotropy in shaping these observational signatures, we analyse here the effects produced by the presence of a population of centrally concentrated stellar-mass black holes. We fit dynamical models to omega Cen data, and we show that models with similar to 5 per cent of their mass in black holes (consistent with similar to 100 per cent retention fraction after natal kicks) can reproduce the data. When simultaneously considering both radial anisotropy and mass segregation, the best-fit model includes a smaller population of remnants, and a less extreme degree of anisotropy with respect to the models that include only one of these features. These results underline that before conclusions about putative IMBHs can be made, the effects of stellar-mass black holes and radial anisotropy need to be properly accounted for.
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