Table D.1
Simulation information.
| Name | Total mass | Sink mass | Magnetization (μ) | Turbulent Mach number | Age |
|---|---|---|---|---|---|
| (M⊙) | (M⊙) | (kyr) | |||
| High-luminosity model I | 100 | 4.1 | 5 | 0 | 39.2 |
| High-luminosity model II | 100 | 3.7 | 5 | 0 | 37.1 |
| High-luminosity model III | 60 | 7.4 | 5 | 0 | 35.6 |
| Low-luminosity model I | 30 | 1.3 | 9 | 2 | 148 |
| Low-luminosity model II (a) | 30 | 2.0 | 9 | 2 | 187 |
| Low-luminosity model III (b) | 30 | 0.8 | 9 | 2 | 153 |
Notes. All the simulations have a spatial resolution of a few au, and implement ambipolar diffusion. The initial density profile is ρ ∝ 1∕(1 + r2) in runs I, II, III, and is uniform in runs IV, V, and VI. For each of them we select a time step at which the simulation exhibits compact features in density similar to those that we see in the ALMA observations, i.e., bright emission from the infalling envelope, disk-like structures, and bipolar outflow cavities. (a) The sink mass is that of the largest central sink. This core is fragmenting, and thus there are several other, smaller sinks. (b) The jet is implemented by hand, with a speedof 66% of the escape speed, and an opening angle of 30°. The corresponding outflowing mass ejected by the sink is 1/3 of the mass accreted by the sink.
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