2013A&A...558A.117L


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.20CET06:58:52

2013A&A...558A.117L - Astronomy and Astrophysics, volume 558A, 117-117 (2013/10-1)

N-body simulations of globular clusters in tidal fields: effects of intermediate-mass black holes.

LUETZGENDORF N., BAUMGARDT H. and KRUIJSSEN J.M.D.

Abstract (from CDS):

Intermediate-mass black holes (IMBHs) may provide the missing link to understanding the growth of supermassive black holes in the early Universe. Some formation scenarios predict that IMBHs could have formed by runaway collisions in globular clusters (GCs). However, it is challenging to set observational constraints on the mass of a black hole in a largely gas-free (and hence accretion-free) stellar system such as a GC. Understanding the influence of an IMBH in the center of a GC on its environment might provide indirect detection methods. Our goal is to test the effects of different initial compositions of GCs on their evolution in a tidal field. We pin down the crucial observables that indicate the presence of an IMBH at the center of the cluster. In addition to central IMBHs, we also consider the effects of different stellar-mass black hole retention and stellar binary fractions. We performed a set of 22 N-body simulations and varied particle numbers, IMBH masses, stellar-mass black-hole retention fractions, and stellar binary fractions. These models are all run in an external tidal field to study the effect of black holes on the cluster mass loss, mass function, and life times. Finally, we compared our results with observational data. We found that a central massive black hole increases the escape rate of high-mass stars from a star cluster, implying that the relative depletion of the mass function at the low-mass end proceeds less rapidly. Furthermore, we found a similar behavior for a cluster hosting a high number of stellar-mass black holes instead of one massive central IMBH. The presence of an IMBH also weakly affects the fraction of the cluster mass that is constituted by stellar remnants, as does the presence of primordial binaries. We compared our simulations with observational data from the literature and found good agreement between our models and observed mass functions and structural parameters of GCs. We exploited this agreement to identify GCs that could potentially host IMBHs.

Abstract Copyright:

Journal keyword(s): black hole physics - stars: kinematics and dynamics - methods: numerical - galaxies: star clusters: general

Simbad objects: 21

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Number of rows : 21

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 288 GlC 00 52 45.24 -26 34 57.4   10 8.13     ~ 890 0
2 NGC 1261 GlC 03 12 16.21 -55 12 58.4   9.79 8.63     ~ 404 0
3 MGG 11 Cl* 09 55 50.2 +69 40 45           ~ 65 0
4 NGC 3201 GlC 10 17 36.82 -46 24 44.9   9.18 8.24     ~ 688 0
5 NGC 5053 GlC 13 16 27.09 +17 42 00.9     9.96     ~ 516 0
6 NGC 5139 GlC 13 26 47.28 -47 28 46.1   6.12 5.33     ~ 2920 0
7 M 3 GlC 13 42 11.62 +28 22 38.2     6.39     ~ 2225 0
8 NGC 5286 GlC 13 46 26.81 -51 22 27.3   9.18 8.31     ~ 344 0
9 NGC 5466 GlC 14 05 27.29 +28 32 04.0   10.5 9.70     ~ 699 0
10 NAME Serpens Dwarf GlC 15 16 05.30 -00 06 41.0   15.1       ~ 601 1
11 NGC 5927 GlC 15 28 00.69 -50 40 22.9   10.13 8.86     ~ 389 0
12 M 80 GlC 16 17 02.41 -22 58 33.9           ~ 595 0
13 M 10 GlC 16 57 09.05 -04 06 01.1     4.98     ~ 654 0
14 M 92 GlC 17 17 07.39 +43 08 09.4     6.52     ~ 1870 0
15 NGC 6397 GlC 17 40 42.09 -53 40 27.6   7.39 5.17     ~ 1756 1
16 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11051 0
17 NGC 6496 GlC 17 59 03.68 -44 15 57.4   9.96       ~ 169 0
18 M 22 GlC 18 36 23.94 -23 54 17.1   7.16 6.17     ~ 1177 0
19 NGC 6712 GlC 18 53 04.32 -08 42 21.5   9.85 8.69     ~ 458 0
20 M 55 GlC 19 39 59.71 -30 57 53.1     6.49     ~ 734 0
21 M 15 GlC 21 29 58.33 +12 10 01.2   3       ~ 2851 0

    Equat.    Gal    SGal    Ecl

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2019.11.20-06:58:52

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