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  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/28914
Title: No evidence for intermediate-mass black holes in the globular clusters ω Cen and NGC 6624
Authors: Baumgardt, H.
He, C.
Sweet, S. M.
Drinkwater, M.
SOLLIMA, ANTONIO LUIGI 
Hurley, J.
Usher, C.
Kamann, S.
Dalgleish, H.
Dreizler, S.
Husser, T. -O.
Issue Date: 2019
Journal: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 
Number: 488
Issue: 4
First Page: 5340
Abstract: We compare the results of a large grid of N-body simulations with the surface brightness and velocity dispersion profiles of the globular clusters ω Cen and NGC 6624. Our models include clusters with varying stellar-mass black hole retention fractions and varying masses of a central intermediate-mass black hole (IMBH). We find that an ∼ 45 000 M<SUB>☉</SUB> IMBH, whose presence has been suggested based on the measured velocity dispersion profile of ω Cen, predicts the existence of about 20 fast-moving, m > 0.5 M<SUB>☉</SUB>, main-sequence stars with a (1D) velocity v > 60 km s<SUP>-1</SUP> in the central 20 arcsec of ω Cen. However, no such star is present in the HST/ACS proper motion catalogue of Bellini et al. (2017), strongly ruling out the presence of a massive IMBH in the core of ω Cen. Instead, we find that all available data can be fitted by a model that contains 4.6 per cent of the mass of ω Cen in a centrally concentrated cluster of stellar-mass black holes. We show that this mass fraction in stellar-mass BHs is compatible with the predictions of stellar evolution models of massive stars. We also compare our grid of N-body simulations with NGC 6624, a cluster recently claimed to harbour a 20 000 M<SUB>☉</SUB> black hole based on timing observations of millisecond pulsars. However, we find that models with M<SUB>IMBH</SUB> > 1000 M<SUB>☉</SUB> IMBHs are incompatible with the observed velocity dispersion and surface brightness profile of NGC 6624, ruling out the presence of a massive IMBH in this cluster. Models without an IMBH provide again an excellent fit to NGC 6624.
URI: http://hdl.handle.net/20.500.12386/28914
URL: https://academic.oup.com/mnras/article/488/4/5340/5539719
ISSN: 0035-8711
DOI: 10.1093/mnras/stz2060
Bibcode ADS: 2019MNRAS.488.5340B
Fulltext: open
Appears in Collections:1.01 Articoli in rivista

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