Table A.1.
Properties of a selection of nearby YMCs from Portegies Zwart et al. (2010).
| Galaxy | Cluster | Distance | Age | log(mass) | Core radius | log10(ρ) | Limiting mass |
|---|---|---|---|---|---|---|---|
| (kpc) | (Myr) | (M⊙) | (arcsec) | (stars arcsec−2) | (M⊙) | ||
| Cores resolvable by the HST | |||||||
| MW | ONC | 0.4 | 1 | 3.7 | 100 | −1.6 | 0.01 |
| Cores resolvable by the JWST | |||||||
| MW | Trumpler-14 | 2.7 | 2 | 4 | 10.7 | 1.1 | 0.01 |
| MW | Quintuplet | 8.5 | 4 | 4.0 | 24 | 1.1 | 0.04 |
| MW | NGC 3603 | 3.6 | 2 | 4.1 | 8.6 | 1.2 | 0.01 |
| MW | Westerlund-1 | 5.2 | 3.5 | 4.5 | 15.9 | 1.7 | 0.01 |
| LMC | NGC 2214 | 50 | 39.8 | 4.0 | 7.5 | 1.9 | 0.1 |
| Cores resolvable by MICADO | |||||||
| LMC | NGC 1847 | 50 | 26.3 | 4.4 | 7.1 | 2.2 | 0.1 |
| LMC | NGC 2157 | 50 | 39.8 | 4.3 | 8.2 | 2.2 | 0.1 |
| LMC | NGC 1711 | 50 | 50.1 | 4.2 | 7.9 | 2.2 | 0.1 |
| LMC | NGC 1818 | 50 | 25.1 | 4.4 | 8.5 | 2.3 | 0.1 |
| LMC | NGC 2164 | 50 | 50.1 | 4.2 | 6.1 | 2.3 | 0.1 |
| SMC | NGC 330 | 63 | 25.1 | 4.6 | 7.7 | 2.4 | 0.15 |
| LMC | NGC 2136 | 50 | 100 | 4.3 | 6.6 | 2.4 | 0.1 |
| MW | Arches | 8.5 | 2 | 4.3 | 4.9 | 2.5 | 0.04 |
| LMC | NGC 1850 | 50 | 31.6 | 4.9 | 11 | 2.5 | 0.1 |
| LMC | NGC 2004 | 50 | 20 | 4.4 | 5.8 | 2.5 | 0.1 |
| LMC | NGC 2100 | 50 | 15.8 | 4.4 | 4.1 | 2.7 | 0.1 |
| M 31 | B257D | 780 | 79.4 | 4.5 | 0.8 | 3.4 | 0.9 |
| Only outer regions resolvable by MICADO | |||||||
| LMC | R136 | 50 | 3 | 4.8 | 0.41 | 3.7 | 0.1 |
| M 31 | B066 | 780 | 70.8 | 4.3 | 0.10 | 4.2 | 0.9 |
| M 31 | B040 | 780 | 79.4 | 4.5 | 0.15 | 4.3 | 0.9 |
| M 31 | B043 | 780 | 79.4 | 4.4 | 0.19 | 4.3 | 0.9 |
| M 31 | B318 | 780 | 70.8 | 4.4 | 0.05 | 4.4 | 0.9 |
| M 31 | B448 | 780 | 79.4 | 4.4 | 0.05 | 4.4 | 0.9 |
| M 31 | Vdb0 | 780 | 25.1 | 4.9 | 0.37 | 4.4 | 0.9 |
| M 31 | B327 | 780 | 50.1 | 4.4 | 0.05 | 4.5 | 0.9 |
| M 31 | B015D | 780 | 70.8 | 4.8 | 0.06 | 4.6 | 0.9 |
Notes. The age and observable stellar densities for a selection of YMCs found both inside and outside the Milky Way, as listed in Portegies Zwart et al. (2010). Only clusters from Portegies Zwart et al. (2010) with a defined core radius, rc, are shown. The densities were calculated to include only stars blefter than Ks = 28m because fainter stars will not be detectable by MICADO. The table lists the parameters for the clusters shown in Fig. 5.
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