Table 5
Intermediate-mass black holes in globular clusters. Constraints from kinematical studies.
| Name | Method | M GC | ϵ M GC | σ 0 | ϵ σ 0 | M IMBH | ϵ MIMBH | Ref. |
| M ⊙ | M ⊙ | km s-1 | km s-1 | M ⊙ | M ⊙ | |||
|
|
||||||||
| 47 Tuc | p.m. | 1.1 × 106 | 1.0 × 105 | 11.5 | 2.3 | < 1.5 × 103 | 1 | |
| NGC 1851 | l.b. | 3.7 × 105 | 2.6 × 104 | 9.3 | 0.5 | < 2.0 × 103 | 2 | |
| NGC 1904 | l.b. | 1.4 × 105 | 1.0 × 104 | 8.0 | 0.5 | 3.0 × 103 | 1.0 × 103 | 2 |
| NGC 2808 | l.b. | 8.5 × 105 | 1.0 × 105 | 13.4 | 2.6 | < 6.0 × 103 | 3 | |
| ω Cen | p.m. | 2.5 × 106 | 2.3 × 105 | 16.0 | 3.2 | < 1.2 × 104 | 4 | |
| ω Cen | l.b. | 2.5 × 106 | 2.3 × 105 | 16.0 | 3.2 | 4.7 × 104 | 1.0 × 104 | 5 |
| NGC 5286 | l.b. | 4.4 × 105 | 1.8 × 104 | 10.0 | 2.0 | 1.5 × 103 | 1.0 × 103 | 6 |
| NGC 5694 | l.b. | 2.6 × 105 | 3.0 × 104 | 8.8 | 0.6 | < 8.0 × 103 | 2 | |
| NGC 5824 | l.b. | 4.5 × 105 | 3.1 × 104 | 11.2 | 0.4 | < 6.0 × 103 | 2 | |
| NGC 6093 | l.b. | 3.4 × 105 | 1.6 × 104 | 9.3 | 0.3 | < 8.0 × 102 | 2 | |
| NGC 6266 | p.m. | 8.2 × 105 | 1.7 × 104 | 13.7 | 1.1 | < 4.0 × 103 | 7 | |
| NGC 6266 | l.b. | 9.3 × 105 | 2.1 × 104 | 15.5 | 0.5 | 2.0 × 103 | 1.0 × 103 | 2 |
| NGC 6388 | l.b. | 1.1 × 106 | 1.7 × 105 | 18.9 | 0.8 | 1.7 × 104 | 9.0 × 103 | 8 |
| NGC 6388 | r.v. | 1.1 × 106 | 1.7 × 105 | 13.0 | 2.0 | < 2.0 × 103 | 9 | |
| M15 | r.v., p.m. | 6.0 × 105 | 4.0 × 104 | 12.0 | 2.0 | < 3.4 × 103 | 10 | |
| G1 | l.b. | 1.1 × 107 | 4.4 × 106 | 25.1 | 1.7 | 1.8 × 104 | 5.0 × 103 | 11 |
| M3 | r.v. | 2.7 × 105 | 3.8 × 104 | 7.9 | 0.7 | < 5.3 × 103 | This study | |
| M13 | r.v. | 4.0 × 105 | 5.2 × 104 | 9.3 | 0.8 | < 8.1 × 103 | This study | |
| M92 | r.v. | 2.3 × 105 | 2.9 × 104 | 8.1 | 0.7 | < 9.8 × 102 | This study | |
Notes. Column 2 contains the method(s) used to infer stellar dynamics: proper motions (p.m.), radial velocities (r.v.), or line broadening (l.b.). The upper limits on IMBH masses are 1σ limits.
Reference. (1) McLaughlin et al. (2006); (2) Lützgendorf et al. (2013); (3) Lützgendorf et al. (2012b); (4) van der Marel & Anderson (2010); (5) Noyola et al. (2010); (6) Feldmeier et al. (2013); (7) McNamara et al. (2012); (8) Lützgendorf et al. (2011); (9) Lanzoni et al. (2013); (10) van den Bosch et al. (2006); (11) Gebhardt et al. (2005).
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