Superbubble dynamics in globular cluster infancy - I. How do globular clusters first lose their cold gas?

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Table 1

Minimum star formation efficiency and half-mass radius for SN feedback to be able to expel the gas.

M_tot^a /10⁶ M_⊙	ϵ _sf,crit,std ^b	ϵ _sf,crit,sn ^c	r_1/2,crit^d/pc

1	0.97	0.47	4
9	>0.99	>0.99	18
20	>0.99	>0.99	35

Notes.

^(a)

Total initial gas mass out of which the cluster forms.

^(b)

Critical star formation efficiency for our standard energy injection scenario and a half-mass radius of 3 pc.

^(c)

Critical star formation efficiency for the “SN only” energy injection scenario and a half-mass radius of 3 pc.

^(d)

Critical half-mass radius in the “SN only” scenario, assuming a star formation efficiency of 0.33.

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