Table 1
Basic present-day (z = 0) characteristics of the 25 simulated disks.
| Suite | Galaxy | MTot | M∗,disk | rdisk | Environment | d[Z∗,all]/dh | d[Z∗,young]/dR |
| (1011M⊙) | (1010M⊙) | (kpc) | (dex/kpc) | (dex/kpc) | |||
|
|
|||||||
| MUGS | g15784 | 14.0 | 5.9 | 3.2 | Field | −0.06 | −0.04 |
| g422 | 9.1 | 2.0 | 2.8 | Field | −0.06 | −0.08 | |
| g1536 | 7.0 | 3.3 | 2.5 | Field | −0.07 | −0.05 | |
| g24334 | 7.7 | 2.7 | 1.0 | Field | −0.03 | −0.19 | |
|
|
|||||||
| GCD + | Gal1 | 8.8 | 4.1 | 2.7 | Field | −0.04 | −0.01 |
|
|
|||||||
| Grape-SPH | KN11 | 11.0 | 2.0 | 4.7 | Field | −0.03 | −0.04 |
|
|
|||||||
| RaDES | Castor | 10.5 | 7.2 | 4.0 | Loose Group | −0.17 | −0.03 |
| Pollux | 4.2 | 3.4 | 3.0 | Loose Group | −0.06 | −0.05 | |
| Tyndareus | 3.3 | 1.3 | 1.3 | Loose Group | −0.02 | −0.05 | |
| Zeus | 2.3 | 1.0 | 1.7 | Loose Group | −0.07 | −0.04 | |
| Apollo | 8.9 | 6.3 | 3.0 | Loose Group | −0.04 | −0.06 | |
| Artemis | 7.5 | 3.2 | 1.9 | Loose Group | −0.08 | −0.05 | |
| Daphne | 3.1 | 2.1 | 2.7 | Loose Group | −0.03 | −0.06 | |
| Leto | 2.5 | 1.2 | 1.8 | Loose Group | −0.04 | −0.05 | |
| Luke | 11.3 | 6.6 | 5.4 | Loose Group | −0.01 | −0.03 | |
| Leia | 3.9 | 3.0 | 4.1 | Loose Group | −0.05 | −0.02 | |
| Tethys | 7.2 | 5.1 | 2.8 | Field | −0.08 | −0.05 | |
| Krios | 5.7 | 4.0 | 2.5 | Field | −0.10 | −0.05 | |
| Atlas | 6.5 | 4.4 | 2.8 | Field | −0.06 | −0.04 | |
| Hyperion | 10.0 | 7.7 | 3.6 | Field | −0.07 | −0.04 | |
| Eos | 4.6 | 2.5 | 2.0 | Field | −0.19 | −0.07 | |
| Helios | 10.5 | 6.6 | 1.6 | Field | −0.11 | −0.04 | |
| Selene | 6.1 | 5.2 | 3.5 | Field | −0.05 | −0.06 | |
| Oceanus | 11.0 | 10.0 | 6.6 | Field | −0.03 | −0.03 | |
| Ben | 7.7 | 4.2 | 3.9 | Field | −0.04 | −0.03 | |
Notes. Column (1): simulation suite to which the the code used to simulate the galaxy (Col. (2)) belongs; Col. (3): total (dynamical) mass within the virial radius; Col. (4): mass of the stellar disk, after application of the kinematic and spatial cuts described in Sect. 3; Col. (5): exponential scalelength of the stellar disk; Col. (6): local environment of the galaxy; Col. (7): mass-weighted vertical stellar abundance gradient, averaged over the radial range 1.5 < rdisk < 2.5; Col. (8): mass-weighted radial young(stars born within the past 100 Myr) stellar abundance gradient, after application of the kinematic and spatial cuts described in Sect. 3.
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