Table 1.
The fraction of stars in clusters 
for a time-independent SFR for stars younger than 300 Myr.
| β | SFR | Mecl, min | Mecl, max | Spectral | Rg |
 |
|---|---|---|---|---|---|---|
| [M⊙ yr−1] | [M⊙] | [M⊙] | type | [kpc] | ||
| 2.0 | – | 30 | 1.0 × 104 | All | 4 | 0.26 |
| 2.0 | – | 30 | 1.0 × 104 | All | 8 | 0.33 |
| 2.0 | – | 30 | 1.0 × 104 | All | 12 | 0.41 |
| 2.0 | – | 30 | 2.0 × 104 | All | 4 | 0.36 |
| 2.0 | – | 30 | 4.0 × 103 | All | 8 | 0.30 |
| 2.0 | – | 30 | 1.0 × 103 | All | 12 | 0.29 |
| 2.0 | – | 30 | 1.0 × 104 | O-B3 | 8 | 0.83 |
| 2.0 | – | 30 | 1.0 × 104 | B0-B3 | 8 | 0.67 |
| 2.0 | – | 30 | 1.0 × 104 | B3-A0 | 8 | 0.41 |
| 2.0 | – | 30 | 1.0 × 104 | A | 8 | 0.39 |
| 2.0 | – | 30 | 1.0 × 104 | F-K | 8 | 0.35 |
| 2.0 | – | 30 | 1.0 × 104 | M | 8 | 0.32 |
| 1.5 | 0.01 | 5 | 2.7 × 103 | All | 8 | 0.39 |
| 1.5 | 0.10 | 5 | 1.5 × 104 | All | 8 | 0.55 |
| 1.5 | 1.00 | 5 | 8.5 × 104 | All | 8 | 0.72 |
| 1.5 | 10.00 | 5 | 4.8 × 105 | All | 8 | 0.78 |
| 1.5 | 100.00 | 5 | 2.7 × 106 | All | 8 | 0.84 |
| 2.0 | 0.01 | 5 | 2.7 × 103 | All | 8 | 0.24 |
| 2.0 | 0.10 | 5 | 1.5 × 104 | All | 8 | 0.32 |
| 2.0 | 1.00 | 5 | 8.5 × 104 | All | 8 | 0.42 |
| 2.0 | 10.00 | 5 | 4.8 × 105 | All | 8 | 0.47 |
| 2.0 | 100.00 | 5 | 2.7 × 106 | All | 8 | 0.53 |
| 2.4 | 0.01 | 5 | 2.7 × 103 | All | 8 | 0.16 |
| 2.4 | 0.10 | 5 | 1.5 × 104 | All | 8 | 0.17 |
| 2.4 | 1.00 | 5 | 8.5 × 104 | All | 8 | 0.18 |
| 2.4 | 10.00 | 5 | 4.8 × 105 | All | 8 | 0.19 |
| 2.4 | 100.00 | 5 | 2.7 × 106 | All | 8 | 0.19 |
Notes. The data are divided into four groups as indicated by the horizontal lines. The first group of three rows corresponds to the models of Sect. 4.2 with fixed Mecl, max, which are calculated at three different Rg. The second group is for the same models but assuming Mecl, max dependent on the galactocentric radius according to Pflamm-Altenburg & Kroupa (2008). The third group of six rows lists the fraction of stars in clusters according to their spectral type for the models with Rg = 8 kpc. The last group represents the IGIMF models with different ECMF slopes β and SFRs (models of Sect. 4.3). The upper cluster mass limit Mecl, max is a function of the assumed SFR (Eq. (6)).
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