Table 2
Critical star formation efficiency ϵSF,crit for successful gas removal in a certain scenario.
| log(M∗/M⊙)a | rh = 1 pcb | rh = 3 pcb | rh = 10 pcb |
|
|
|||
| Stellar winds at low metallicity, [Fe/H] = −1.5 | |||
| 5 | 0.8 (1.45) | 0.5 (0.73) | 0.3 (0.37) |
| 6 | 0.9 | 0.8 (1.88) | 0.6 (0.63) |
| 7 | 0.9 | 0.9 | 0.9 |
| Stellar winds at solar metallicity | |||
| 5 | 0.4 (1.90) | 0.3 (0.59) | 0 (0.63) |
| 6 | 0.9 | 0.8 (0.84) | 0.4 (0.46) |
| 7 | 0.9 | 0.9 | 0.8 (0.63) |
| Normal supernovae, E0 = 1051 erg | |||
| 5 | 0.5 (0.66) | 0.2 (0.55) | 0 (0.54) |
| 6 | 0.9 | 0.7 (0.52) | 0.4 (0.37) |
| 7 | 0.9 | 0.9 | 0.8 (0.42) |
| Hypernovae, E0 = 1052 erg | |||
| 5 | 0.2 (0.64) | 0 ( 0.72) | 0 (0.25) |
| 6 | 0.7 (0.56) | 0.3 (0.61) | 0.1 (0.43) |
| 7 | 0.9 | 0.8 (0.52) | 0.4 (0.55) |
| Hypernovae, E0 = 1053 erg | |||
| 5 | 0 (0.80) | 0 (0.31) | 0 (0.11) |
| 6 | 0.3 (0.64) | 0.1 (0.56) | 0 (0.36) |
| 7 | 0.8 (0.67) | 0.5 (0.55) | 0.1 (0.65) |
Notes. Given is ϵSF of the last model that did not result in successful gas expulsion, where ϵSF was varied in steps of 0.1, or 0 if all investigated models lead to gas expulsion. If the number is lower than 0.9, we give the gas removal timescale at a star formation efficiency higher by ΔϵSF,crit = 0.1 in units of the crossing time in brackets. .
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