Table 1.
Main simulation parameters used in our runs.
| ID | m* [M⊙] | t* [Myr] | ϵSF | ϵB, SF | ξSF | αB, cold | αB, hot | fk, cold | fk, hot | ϵB, AGN | ξAGN | B1 Mpc [nG] | ξe(ℳ) |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (a) | (b) | (c) | (d) | (e) | (f) | (g) | (h) | (i) | (j) | (k) | (l) | (m) | (n) |
| A1 | 107 | 10 | 10−8 | 0.1 | 10−5 | 1 | 10 | 0.18 | 0.81 | 0.1 | 10−3 | 10−7 | Eq. (3) |
| A2 | 107 | 10 | 10−8 | 0.1 | 10−5 | 1 | 50 | 0.18 | 0.81 | 0.1 | 10−3 | 10−7 | Eq. (3) |
| B1 | 3 ⋅ 107 | 10 | 3 ⋅ 10−8 | 0.1 | 10−5 | 1 | 10 | 0.18 | 0.81 | 0.1 | 10−3 | 10−7 | Eq. (3) |
| B2 | 5 ⋅ 107 | 10 | 5 ⋅ 10−8 | 0.1 | 10−5 | 1 | 10 | 0.18 | 0.81 | 0.1 | 10−3 | 10−7 | Eq. (3) |
| B3 | 3 ⋅ 107 | 30 | 3 ⋅ 10−8 | 0.1 | 10−5 | 1 | 10 | 0.18 | 0.81 | 0.1 | 10−3 | 10−7 | Eq. (3) |
| B4 | 3 ⋅ 107 | 20 | 3 ⋅ 10−8 | 0.1 | 10−5 | 1 | 10 | 0.18 | 0.81 | 0.1 | 10−3 | 10−7 | Eq. (3) |
| C1 | 3 ⋅ 107 | 20 | 3 ⋅ 10−8 | 0.1 | 10−5 | 1 | 10 | 0.18 | 0.81 | 0.1 | 10−3 | 0.37, k−1 | Eq. (3) |
| C2 | 3 ⋅ 107 | 20 | 3 ⋅ 10−8 | 0.1 | 10−5 | 1 | 10 | 0.18 | 0.81 | 0.1 | 10−3 | 0.37, k−1 | Eq. (3), θB ≥ 45° |
Notes. Each column gives: (a) the run ID used in the paper, (b) the minimum mass of star-forming particles; (c) the minimum timescale for forming star particles; (d) the efficiency of stellar feedback (referred to the accreted rest mass energy); (e) the efficiency of magnetic feedback (referred to the feedback energy); (f) the acceleration efficiency of CRe by stellar feedback; (g) the used boost parameter in Bondi accretion formula for cold gas; (h) the used boost parameter in Bondi accretion formula for hot gas; (i) the fraction of feedback energy assigned to kinetic feedback in the cold accretion mode; (j) the fraction of feedback energy assigned to kinetic feedback in the hot accretion mode; (k) the efficiency of magnetic feedback energy (referred to the total feedback energy); (l) the acceleration efficiency of CRe by AGN feedback; (m) the average initial magnetic field amplitude smoothed on a comoving 1 Mpc; (n) the assume injection efficiency by shocks. Relevant parameters which were instead kept the same for all runs were: the physical gas density for star formation, nSF = 10−3 part/cm3, the comoving density for the SMBH simulation, 
, the assumed fixed temperature in the Bondi-Hoyle accretion rate, TAGN = 105 K. We mark model B4 in boldface as the one overall best performing in our suite of runs.
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