Table 2.
Open in new tab

Overview of the four models we use for primordial star formation. The fiducial model assumes an IMF from 3 to 300 M⊙ and only pristine gas can form Pop III stars. In the second model, we change the IMF to slightly lower masses from 1 to 100 M⊙. The third model allows Pop III star formation up to a metallicity of Zcrit = 10−3.5. In the last model, we determine the stellar mass per halo based on the merger history. In all the models, we calibrate the SFE to reproduce the optical depth to Thomson scattering.

LabelMminMmaxSFEZcrit
Fiducial3 M⊙300 M⊙Equation (5), η = 0.140
1→1001 M⊙100 M⊙Equation (5), η = 0.200
Zcrit3 M⊙300 M⊙Equation (5), η = 0.1210−3.5
Merger3 M⊙300 M⊙Equation (8), ϵ1 : 1 = 4 × 10−30
LabelMminMmaxSFEZcrit
Fiducial3 M⊙300 M⊙Equation (5), η = 0.140
1→1001 M⊙100 M⊙Equation (5), η = 0.200
Zcrit3 M⊙300 M⊙Equation (5), η = 0.1210−3.5
Merger3 M⊙300 M⊙Equation (8), ϵ1 : 1 = 4 × 10−30
Table 2.
Open in new tab

Overview of the four models we use for primordial star formation. The fiducial model assumes an IMF from 3 to 300 M⊙ and only pristine gas can form Pop III stars. In the second model, we change the IMF to slightly lower masses from 1 to 100 M⊙. The third model allows Pop III star formation up to a metallicity of Zcrit = 10−3.5. In the last model, we determine the stellar mass per halo based on the merger history. In all the models, we calibrate the SFE to reproduce the optical depth to Thomson scattering.

LabelMminMmaxSFEZcrit
Fiducial3 M⊙300 M⊙Equation (5), η = 0.140
1→1001 M⊙100 M⊙Equation (5), η = 0.200
Zcrit3 M⊙300 M⊙Equation (5), η = 0.1210−3.5
Merger3 M⊙300 M⊙Equation (8), ϵ1 : 1 = 4 × 10−30
LabelMminMmaxSFEZcrit
Fiducial3 M⊙300 M⊙Equation (5), η = 0.140
1→1001 M⊙100 M⊙Equation (5), η = 0.200
Zcrit3 M⊙300 M⊙Equation (5), η = 0.1210−3.5
Merger3 M⊙300 M⊙Equation (8), ϵ1 : 1 = 4 × 10−30
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