Table 6:
The properties of young massive clusters taken from the literature.
Galaxy |
ID |
Age |
age |
 |
 |
 |
 |
  |
Referencea |
|
|
(log yr) |
(log yr) |
(mag) |
(pc) |
(pc) |
(km s-1) |
(km s-1) |
|
Young Massive Star Clusters |
|
|
|
|
|
|
|
|
|
M 82 |
F |
7.6(6.6) |
0.17 |
-14.2 |
1.5 |
0.5 |
13.4 |
0.7 |
1, 10 |
M 82 |
MGG9 |
6.9 |
0.15 |
-13.43 |
2.6 |
0.4 |
15.9 |
0.8 |
4 |
M 82 |
MGG11 |
6.9 |
0.15 |
-13.23 |
1.2 |
0.17 |
11.4 |
0.8 |
4 |
NGC 1569 |
A |
7.08 |
0.2 |
-14.1 |
1.9 |
0.2 |
15.7 |
1.5 |
7, 8 |
NGC 1705 |
1 |
7.08 |
0.2 |
-14.0 |
1.6 |
0.2 |
11.4 |
1.5 |
1, 9 |
NGC 4038 |
W99-15 |
6.93 |
0.2 |
-13.69 |
3.6 |
0.5 |
20.2 |
0.7 |
6 |
NGC 4038 |
W99-2 |
6.95 |
0.2 |
-14.79 |
4.5 |
0.5 |
14.2 |
0.4 |
6 |
NGC 4038 |
W99-1 |
6.91 |
0.2 |
-14.0 |
3.6 |
0.5 |
9.1 |
0.6 |
6 |
NGC 4038 |
W99-16 |
7.0 |
0.1 |
-12.70 |
6.0 |
0.5 |
15.8 |
1.0 |
6 |
NGC 4214 |
10 |
8.3 |
0.1 |
-10.22 |
4.33 |
0.1 |
5.1 |
1.0 |
3 |
NGC 4214 |
13 |
8.3 |
0.1 |
-11.68 |
3.01 |
0.2 |
14.8 |
1.0 |
3 |
NGC 4449 |
27 |
8.9 |
0.25 |
-9.61 |
3.72 |
0.32 |
5.0 |
1.0 |
3 |
NGC 4449 |
47 |
8.45 |
0.10 |
-10.74 |
5.24 |
0.76 |
6.2 |
1.0 |
3 |
NGC 5236 |
502 |
8.0 |
0.1 |
-11.57 |
7.6 |
1.1 |
5.5 |
0.2 |
2 |
NGC 5236 |
805 |
7.1 |
0.2 |
-12.17 |
2.8 |
0.4 |
8.1 |
0.2 |
2 |
NGC 6946 |
1447 |
7.05 |
0.10 |
-14.17 |
10.2 |
1.6 |
8.8 |
1.0 |
3 |
NGC 1316 |
G114 |
9.47 |
0.1 |
-13.0 |
4.1 |
0.25 |
42.1 |
2.8 |
this work |
NGC 7252 |
W30 |
8.6 |
0.1 |
-14.6 |
9.3 |
1.7 |
27.5 |
2.5 |
this work |
NGC 7252 |
W3 |
8.6 |
0.1 |
-16.2 |
17.5 |
1.8 |
45 |
5.0 |
5 |
Nuclear Star Clusters |
|
|
|
MIb |
|
|
|
|
|
NGC 300 |
- |
- |
- |
-11.4 |
2.9 |
- |
13.3 |
2.0 |
11, 12 |
NGC 428 |
- |
- |
- |
-13.1 |
3.4 |
- |
24.4 |
3.7 |
11, 12 |
NGC 1042 |
- |
- |
- |
-13.1 |
1.9 |
- |
32.0 |
4.8 |
11, 12 |
NGC 1493 |
- |
- |
- |
-13.1 |
2.6 |
- |
25.0 |
3.8 |
11, 12 |
NGC 3423 |
- |
- |
- |
-11.8 |
4.2 |
- |
30.4 |
4.6 |
11, 12 |
NGC 7793 |
- |
- |
- |
-13.6 |
7.7 |
- |
24.6 |
3.7 |
11, 12 |
- a
- References: 1) Smith & Gallagher (2001); 2)
Larsen & Richtler (2004); 3) Larsen et al. (2004); 4) McCrady et al. (2003); 5) Maraston et al. (2004); 6) Mengel et al. (2002); 7) Ho
& Filippenko (1996b); 8) Anders et al. (2004); 9) Ho &
Filippenko (1996a); 10) McCrady et al. (2005); 11) Böker et al. (2004); 12) Walcher et al. (2005).
- b
- For Fig. 7 we have assumed (B-I)=1.0which corresponds to a simple stellar population of
400 Myr and
solar metallicity, although we note that the assumed (B-I)colour does not change the conclusions.
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