2011A&A...529A.138B


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST18:52:39

2011A&A...529A.138B - Astronomy and Astrophysics, volume 529A, 138-138 (2011/5-1)

A parametric study on the formation of extended star clusters and ultra-compact dwarf galaxies.

BRUNS R.C., KROUPA P., FELLHAUER M., METZ M. and ASSMANN P.

Abstract (from CDS):

In the last decade, very extended old stellar clusters with masses in the range from a few 104 to 108M have been found in various types of galaxies in different environments. Objects with masses comparable to normal globular clusters (GCs) are called extended clusters (ECs), while objects with masses in the dwarf galaxy regime are called ultra-compact dwarf galaxies (UCDs). In heavily interacting galaxies star clusters tend to form in larger conglomerations called star cluster complexes (CCs). The individual star clusters in a CC can merge and form a variety of spheroidal stellar objects. The parametric study aims to analyze how the structural parameters of the final merger objects correlate with the underlying CC parameter space. In this work we systematically scan a suitable parameter space for CCs and perform numerical simulations to study their further fate. The varied sizes and masses of the CCs cover a matrix of 5x6 values with CC Plummer radii between 10-160 pc and CC masses between 105.5-108M, which are consistent with observed CC parameters. The CCs of the parametric study are on orbits with galactocentric distances between 20kpc and 60kpc. In addition, we studied also the evolution of CCs on a circular orbit at a galactocentric distance of 60kpc to verify that also extremely extended ECs and UCDs can be explained by our formation scenario. All 54 simulations end up with stable merger objects, wherein 26 to 97% of the initial CC mass is bound. The objects show a general trend of increasing effective radii with increasing mass. Despite the large range of input Plummer radii of the CCs (10 to 160pc) the effective radii of the merger objects are constrained to values between 10 and 20pc at the low mass end and to values between 15 and 55pc at the high mass end. The structural parameters of the models are comparable to those of the observed ECs and UCDs. The results of the circular orbits demonstrate that even very extended objects like the M31 ECs found by Huxor in 2005 and the very extended (reff>80pc), high-mass UCDs can be explained by merged cluster complexes in regions with low gravitational fields at large galactocentric radii. We conclude that the observed ECs and UCDs can be well explained as evolved star cluster complexes.

Abstract Copyright:

Journal keyword(s): galaxies: star clusters: general - methods: numerical

CDS comments: W3 = [WSL93] 3

Simbad objects: 36

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Number of rows : 36

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 NAME Sculptor dE1 GiG 00 23 51.7 -24 42 18   17.73       ~ 54 1
2 NAME Cartwheel G 00 37 41.107 -33 42 58.79   19.26   18.52   ~ 252 1
3 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 10905 1
4 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5135 1
5 NGC 922 EmG 02 25 04.400 -24 47 17.46   12.54 12.21 11.84   ~ 125 0
6 NAME Fornax Dwarf Spheroidal G 02 39 59.3 -34 26 57   9.02 7.4     ~ 1473 1
7 NGC 1023 IG 02 40 24.012 +39 03 47.70 10.91 10.35 9.35 7.83   ~ 601 2
8 NGC 1380 GiP 03 36 27.590 -34 58 34.68 11.32 10.94 9.93 9.37   ~ 378 1
9 ACO S 373 ClG 03 38 30 -35 27.3           ~ 1538 0
10 NGC 1487 GiP 03 55 46.5 -42 22 01   12.28 11.68 11.74 11.02 ~ 102 0
11 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14832 1
12 NGC 2419 GlC 07 38 08.51 +38 52 54.9     10.05     ~ 815 0
13 M 81 Sy2 09 55 33.17306143 +69 03 55.0609270   7.89 6.94     ~ 3965 5
14 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5336 6
15 APG 24 G 10 54 40.1 +56 59 11           ~ 78 0
16 NAME Antennae IG 12 01 53.170 -18 52 37.92           ~ 1556 0
17 M 85 GiP 12 25 24.053 +18 11 27.89   10.2       ~ 603 0
18 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5825 0
19 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6213 3
20 M 104 LIN 12 39 59.43185 -11 37 22.9954 9.51 9.55 8.00 8.05   ~ 1275 3
21 ACO 3526 ClG 12 48 51.8 -41 18 21           ~ 971 2
22 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4208 2
23 ACO 1689 ClG 13 11 29.5 -01 20 28           ~ 1022 0
24 NAME Centaurus A Sy2 13 25 27.61509104 -43 01 08.8056025   8.18 6.84 6.66   ~ 3999 3
25 M 51 GiP 13 29 52.698 +47 11 42.93   9.26 8.36 8.40   ~ 3782 4
26 M 83 SBG 13 37 00.919 -29 51 56.74 8.85 8.11 7.52 7.21   ~ 2229 2
27 ACO S 740 ClG 13 43 32 -38 11.1           ~ 15 0
28 M 101 GiP 14 03 12.583 +54 20 55.50   8.46 7.86 7.76   ~ 2546 2
29 VV 29 IG 16 06 03.940 +55 25 31.33   15.0       ~ 105 0
30 NGC 6745 G 19 01 41.192 +40 44 37.34   13.3       ~ 69 1
31 NGC 6822 G 19 44 56.199 -14 47 51.29   18 8.1     ~ 1430 0
32 NGC 6946 H2G 20 34 52.332 +60 09 13.24   10.5       ~ 2235 2
33 [WSL93] 3 GlC 22 20 43.878 -24 40 37.87     17.86     ~ 49 0
34 NAME Stephan's Quintet CGG 22 35 57.5 +33 57 36           ~ 375 1
35 NGC 7673 EmG 23 27 41.060 +23 35 20.18 12.84 13.17 12.76     ~ 263 1
36 NAME Local Group GrG ~ ~           ~ 6973 0

    Equat.    Gal    SGal    Ecl

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2020.07.14-18:52:39

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