2004/10/25 by Holger Baumgardt, Junichiro Makino, Piet Hut · 13 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Galaxies: Formation, Evolution, Phenomena #astro-ph
paper · pdf · doi:10.1086/426893
published as Astrophys.J. 620 (2005) 238-243 · 13 pages, 3 figures, Accepted ofr publication in ApJ (scheduled for February 2005)
arxiv created 2004/10/25 · openalex publication_date 2005/02/09 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31
It has been assumed that intermediate-mass black holes (IMBHs) in globular clusters can only reside in the most centrally concentrated clusters, with a so-called core-collapsed density profile. While this would be a natural guess, it is in fact wrong. We have followed the evolution of star clusters containing IMBHs with masses between 125 ≤ M BH ≤ 1000 M ☉ through detailed N -body simulations, and we find that a cluster with an IMBH, in projection, appears to have a relatively large "core" with surface brightness only slightly rising toward the center. This makes it highly unlikely that any of the "core-collapsed" clusters will harbor an IMBH. On the contrary, the places to look for an IMBH are those clusters that can be fitted well by medium-concentration King models. The velocity dispersion of the visible stars in a globular cluster with an IMBH is nearly constant well inside the apparent core radius. For a cluster of mass M C containing an IMBH of mass M BH , the influence of the IMBH becomes significant only at a fraction 2.5 M BH / M C of the half-mass radius, deep within the core, where it will affect only a small number of stars. In conclusion, observational detection of an IMBH may be possible, but will be challenging.