Table 2
Values of the initial radii of the embedded star clusters, Rcl, (Marks & Kroupa 2012), α3 values (see Eq. (3)), and the number of massive stars N(m⋆ > 8 M⊙) computed as a function of initial stellar mass, MUCD = Mecl, and metallicity.
| MKDP IMF | CAN IMF | ||||||
| [Fe/H] = –2 | [Fe/H] = 0 | ||||||
| MUCD [M⊙] | Rcl [pc] | α 3 | 105N(m⋆ > 8 M⊙) | α 3 | 105N(m⋆ > 8 M⊙) | α 3 | 105N(m⋆ > 8 M⊙) |
|
|
|||||||
| 106 | 0.6 | 1.61 | 0.2 | 1.73 | 0.2 | 2.3 | 0.1 |
| 107 | 0.8 | 1.37 | 2.4 | 1.48 | 2.4 | 2.3 | 1.1 |
| 108 | 1.1 | 1.12 | 23.2 | 1.23 | 23.8 | 2.3 | 10.9 |
| 109 | 1.5 | 0.87 | 213.8 | 0.99 | 222.7 | 2.3 | 109.1 |
| 1010 | 2.0 | 0.62 | 1943.1 | 0.74 | 2032.6 | 2.3 | 1091.2 |
Notes. For comparison, we also show N(m⋆ > 8 M⊙) for the CAN IMF. The predicted values of the embedded cluster/UCD initial radii, Rcl, are small. However, due to stellar and dynamical evolution, UCDs expand by approximately a factor of ten (Dabringhausen et al. 2010). We use the Rcl values as an empirical extrapolation from GCs and therefore at UCD scales departures are possible.
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