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Fig. 5


Shell kinematics for cluster 23 in ESO 338-IG04 for the case where the energy is produced by stellar winds and a star formation efficiency of 90 per cent. The meaning of the lines is the same as in Fig. 3, except for the blue dotted lines, which give the observed radius (upper panel) and velocity (middle panel) of the supershell around this object. The low observed velocity compared to our model would mean that most of the observed shell mass would be contributed by ISM around the cluster rather than gas that was originally deep inside its potential well.

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