Table 2.
NOCTUA suite of simulations.
| Simulation | Run time | MBH [M⊙] | SNII | ISR | Lreduce [%] |
|---|---|---|---|---|---|
| Stellar Feedback | |||||
| MBH4_noFB | 800 Myr | 104 | – | – | – |
| MBH4_SNII | 800 Myr | 104 | ✓ | – | – |
| MBH4_ISR | 800 Myr | 104 | – | ✓ | – |
| MBH4_full | 800 Myr | 104 | ✓ | ✓ | – |
| Black Hole Mass | |||||
| MBH3 | 800 Myr | 103 | ✓ | – | – |
| MBH5 | 800 Myr | 105 | ✓ | – | – |
| MBH6 | 300 Myr | 106 | ✓ | – | – |
| Artificial Inflows | |||||
| MBH4_L20 | 300 Myr | 104 | ✓ | – | 20 |
| MBH4_L50 | 300 Myr | 104 | ✓ | – | 50 |
| MBH6_L20 | 300 Myr | 106 | ✓ | – | 20 |
Notes. The simulations are divided into different subsets depending on the scientific question they aim to address (described in more detail in Sect. 2.6): Stellar Feedback for when gradually adding stellar feedback processes to the numerical set-up; Black Hole Mass for when varying the MBH initial mass between 103−6 M⊙; Artificial Inflows for when manually reducing the angular momentum of the gas in the low-mass dwarf galaxy by Lreduce, to induce artificial inflows towards the galactic centre and the central MBH (see Sect. 4.2 for more details on this).
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