SIEGE - III. The formation of dense stellar clusters in sub-parsec resolution cosmological simulations with individual star feedback

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Table 1

Summary of the simulations run in this work.

Model name	Pre-SN feedback (ejection)	IMF	SF efficiency ɛ_ff	Maximum resolution⁽¹⁾	Stellar mass at z = 10.5	Other properties (common to all models)
FC22	Instantaneous	Kroupa (2001)	0.1	0.2 pc	1.7 × 10⁶ M_ʘ	Individual star mass range:
Winds, SFE=0.1	Continuous	Kroupa (2001)	0.1	0.2 pc	3.5 × 10⁶ M_ʘ	>1.5 M_ʘ
Winds, SFE=1.0-LR	Continuous	Kroupa (2001)	1.0	0.8 pc	7.6 × 10⁶ M_ʘ	Massive stars range:
Winds, SFE=1.0	Continuous	Kroupa (2001)	1.0	0.2 pc	5.8 × 10⁶ M_ʘ	8-40 M_ʘ
Winds, THIMF	Continuous	$\frac{d n}{d l o g m} \propto$ $\frac{dn}{dlog m}\propto$ const.	0.1	0.2 pc	1.7 × 10⁶ M_ʘ	M_ej⁽²⁾=0.9 m_ini
						Stellar lifetimes: C15

Notes. ⁽¹⁾Computed at z=15.5, corresponding approximately to the onset of star formation. ⁽²⁾Total mass ejected by massive stars at the end of their lives.

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