Table 1
Summary of the parameters adopted in the simulations used in this work.
| Run | Vvir (km s−1) | c | fgas | MC | Res. | ϵ (pc) | M★ × 1010 (M⊙) | Mh × 1010 (M⊙) | Mgas × 1010 (M⊙) | SFR × 10−2 (M⊙ yr−1) | re,★ (kpc) | re,gas (kpc) |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| 13 | 150 | 6 | 0.3 | Yes | Low | 100 | 3.6 | 139.7 | 0.9 | 4.9 | 2.7 | 4.8 |
| 16 | 150 | 10 | 0.3 | No | Low | 100 | 3.7 | 125.9 | 0.8 | 6.3 | 2.2 | 3.9 |
| 23 | 150 | 10 | 0.3 | Yes | High | 100 | 3.7 | 125.9 | 0.8 | 6.2 | 2.0 | 4.0 |
| 25 | 150 | 10 | 0.5 | No | High | 100 | 3.6 | 125.9 | 0.9 | 23.1 | 2.0 | 5.4 |
| 26 | 150 | 10 | 0.5 | Yes | High | 50 | 3.8 | 125.9 | 0.8 | 5.6 | 1.9 | 5.9 |
| 27 | 180 | 6 | 0.5 | No | Low | 100 | 5.9 | 241.4 | 1.9 | 50.2 | 2.5 | 6.9 |
Notes. The first column reports the number of the run (following the original numbering by Tamburello et al. 2015), the second column displays the velocity at virial radius (Vvir), the third column shows the concentration (c), the fourth column the gas fraction ( fgas) at the initial conditions, the fifth column whether metal cooling (MC) is included or not, the sixth column whether low or high resolution is used (i.e., how many particles are used), the seventh column reports the chosen gravitational softening length (ϵ), the eighth, ninth, and tenth columns report the stellar mass (M★), the halo mass (Mh), and the gas mass (Mgas) after ∆t = 2 Gyr from the end of the relaxation phase, respectively, the eleventh column shows the SFR after ∆t = 2 Gyr from the end of the relaxation phase, and the twelfth and thirteenth columns list the stellar half-mass radius (re,★) and gas half-mass radius (re,gas) after ∆t = 2 Gyr from the end of the relaxation phase, respectively. The halo virial mass of run 13 is different from the other runs with Vvir = 150 km s−1 because the initial conditions are assumed at different redshift from the ARGO simulations, as explained in Sect. 2.
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