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Table 1

Observational data and results of gas expulsion simulations for the YMC sample of Bastian et al. (2014).

Galaxy Cluster Agea M ∗ b r h c C 5 d Z e Ex/ Ex/ ϵ SF,W,c g t ex,w h
(Myr) (105 M⊙) (pc) (Z⊙) Wf SNf (%) (Myr)
NGC 6946 1447 12 ± 2.5 8 17.4 0.46 0.5 Y Y 20 0.63
NGC 1569 A 6 ± 1 7.6 1.5 5.1 0.4 N N 80 0.12
B 15 ± 5 14 2.4 5.9 0.4 N N 80 0.13
NGC 1705 1 12.5 ± 2.5 11 1.5 7.3 0.33 N N 80 0.12
NGC 1140 1 5 ± 1 11 14 0.79 0.5 Y Y 30 0.48
The Antennae T352/W38220 4 ± 2 9.2 4.1 2.2 1 N N 40 0.20
Knot S 5 ± 1 16 14 1.1 1 N Y 40 0.52
ESO 338-IG04 Cluster 23 50 8.9 5.6 0.2 N N 80 0.22

Notes.

(h)

Time since the coeval starburst at which an eventually escaping shell crosses the half-mass radius, for the stellar wind case with ϵSF,W,c.

(a)

Age in Myr.

(b)

Fiducial stellar mass, adopting the photometric mass estimate from Bastian et al. (2014).

(c)

rh: half-mass radius, calculated from the half-light radius assuming a Plummer sphere.

(d)

Compactness index C5 = (M∗/105 M⊙)(rh/pc)-1.

(e)

Metallicity.

(f)

Success of gas expulsion assuming 30 per cent star formation efficiency by, respectively, stellar winds (Ex/W) and supernovae (Ex/SN). Y: yes, N: no.

(g)

Critical star formation efficiency for gas expulsion in the metallicity dependent massive-star wind scenario. With this efficiency, a supershell would just not yet escape. The simulation at a star formation efficiency ten percentiles higher then features successful gas expulsion.

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