Table 1.
Overview of the parameter set of cosmological zoom-in simulation runs.
| Model no. | zf | log Mvir | λ | vwind | Mseed | MHaloMin | BH present |
|---|---|---|---|---|---|---|---|
| [M⊙] | [km s−1] | [M⊙] | [M⊙] | ||||
| NoBHL | 2 | ∼10 | ∼0.035 | N/A | N/A | N/A | No |
| BHs4hl6v2L | 2 | ∼10 | ∼0.035 | 2000 | 5 × 104 | 106 | Yes |
| BHs4hl7v2L | 2 | ∼10 | ∼0.035 | 2000 | 5 × 104 | 107 | Yes |
| BHs4hl6v10L | 2 | ∼10 | ∼0.035 | 10 000 | 5 × 104 | 106 | Yes |
| BHs4hl7v10L | 2 | ∼10 | ∼0.035 | 10 000 | 5 × 104 | 107 | Yes |
| BHs3hl6v2L | 2 | ∼10 | ∼0.035 | 2000 | 5 × 103 | 106 | Yes |
| BHs3hl7v2L | 2 | ∼10 | ∼0.035 | 2000 | 5 × 103 | 107 | Yes |
| BHs3hl6v10L | 2 | ∼10 | ∼0.035 | 10 000 | 5 × 103 | 106 | Yes |
| BHs3hl7v10L | 2 | ∼10 | ∼0.035 | 10 000 | 5 × 103 | 107 | Yes |
| NoBHH | 2 | ∼10 | ∼0.1 | N/A | N/A | N/A | No |
| BHs4hl6v2H | 2 | ∼10 | ∼0.1 | 2000 | 5 × 104 | 106 | Yes |
| BHs4hl7v2H | 2 | ∼10 | ∼0.1 | 2000 | 5 × 104 | 107 | Yes |
| BHs4hl6v10H | 2 | ∼10 | ∼0.1 | 10 000 | 5 × 104 | 106 | Yes |
| BHs4hl7v10H | 2 | ∼10 | ∼0.1 | 10 000 | 5 × 104 | 107 | Yes |
| BHs3hl6v2H | 2 | ∼10 | ∼0.1 | 2000 | 5 × 103 | 106 | Yes |
| BHs3hl7v2H | 2 | ∼10 | ∼0.1 | 2000 | 5 × 103 | 107 | Yes |
| BHs3hl6v10H | 2 | ∼10 | ∼0.1 | 10 000 | 5 × 103 | 106 | Yes |
| BHs3hl7v10H | 2 | ∼10 | ∼0.1 | 10 000 | 5 × 103 | 107 | Yes |
Notes. The simulations with galaxies in low (upper) and high (lower) spin halos are listed separately. The details of our model naming rules can be found in Section 2.3. We list the host DM halo mass (Mvir), spin (λ), AGN wind velocity (vwind), BH initial mass (Mseed) and minimum halo mass for BH seeding (MHaloMin). The gravitational/torque/angular-momentum-driven BH accretion model (Hopkins & Quataert 2011) has been used. Following the observations and theoretical models suggestion, we set all AGN wind models with mass loading β = 1.
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