Table A.1
Properties of the six most massive accreted galaxies and of the in situ component at z=0 for the four MW-like galaxies from the Auriga simulations studied here.
| Halo 21 | |||||
|---|---|---|---|---|---|
| Progenitor | Merger ratio | M⋆(< R200) [109 M⊙] | M⋆(Rhelio < 2.5 kpc) [107 M⊙] | zacc,5–50–90 | State |
| Total | 92.30 | 144.609 | |||
| In situ | 72.88 (79.0%) | 136.789 (94.6%) | |||
| Prog. 1 | 6:1 (2:1) | 9.58 (10.4%) | 4.454 (3.1%) | [1.0, 0.8, 0.8] | M |
| Prog. 2 | 8:1 (2.5:1) | 4.64 (5.0%) | 3.100 (2.1%) | [1.1, 1.0, 1.0] | M |
| Prog. 3* | 20:1 (25:1) | 3.00 (3.2%) | 0.191 (0.1%) | [0.1, 0.1, 0.0] | St |
| Prog. 4* | 12:1 (11:1) | 1.32 (1.4%) | 0.006 (0.0%) | [0.3, 0.1, 0.0] | St |
| Prog. 5 | 36:1 (40:1) | 0.25 (0.3%) | 0.001 (0.0%) | [1.0, 1.0, 0.4] | St |
| Prog. 6* | 43:1 (57:1) | 0.15 (0.2%) | 0.000 (0.0%) | [0.8, 0.3, 0.1] | St |
| Other prog. | 0.048 (0.5%) | 1.0 (0.1%) | [5.5, 1.0, 0.2] | ||
| Halo 23 | |||||
| Progenitor | Merger ratio | M⋆(< R200) [109 M⊙] | M⋆(Rhelio < 2.5 kpc) [107 M⊙] | zacc,5–50–90 | State |
| Total | 93.33 | 138.237 | |||
| in situ | 78.95 (84.6%) | 127.304 (92.1%) | |||
| Prog. 1 | 16:1 (15:1) | 5.57 (6.0%) | 6.154 (4.5%) | [0.6, 0.3, 0.2] | D |
| Prog. 2 | 22:1 (5:1) | 4.94 (5.3%) | 3.687 (2.7%) | [1.8, 1.7, 1.5] | M |
| Prog. 3 | 7:1 (3:1) | 1.03 (1.1%) | 0.265 (0.2%) | [3.1, 2.7, 2.7] | M |
| Prog. 4* | 53:1 (84:1) | 0.69 (0.7%) | 0.001 (0.0%) | [0.6, 0.2, 0.0] | St |
| Prog. 5 | 114:1 (41:1) | 0.41 (0.4%) | 0.338 (0.2%) | [1.8, 1.8, 1.8] | M |
| Prog. 6* | 47:1 (121:1) | 0.28 (0.3%) | 0.000 (0.0%) | [0.8, 0.2, 0.0] | St |
| Other prog. | 1.46 (1.6%) | 0.489 (0.4%) | [4.4, 1.8, 0.2] | ||
| Halo 24 | |||||
| Progenitor | Merger ratio | M⋆(< R200) [109 M⊙] | M⋆(Rhelio < 2.5 kpc) [107 M⊙] | zacc,5–50–90 | State |
| Total | 89.89 | 114.400 | |||
| In situ | 77.32 (86.0%) | 105.676 (92.4%) | |||
| Prog. 1 | 18:1 (17:1) | 4.27 (4.8%) | 3.729 (3.3%) | [0.5, 0.2, 0.2] | D |
| Prog. 2 | 10:1 (8:1) | 3.13 (3.5%) | 2.655 (2.3%) | [1.2, 1.2, 1.2] | M |
| Prog. 3 | 51:1 (4:1) | 2.00 (2.2%) | 0.977 (0.9%) | [2.0, 1.7, 1.7] | M |
| Prog. 4 | 29:1 (23:1) | 0.80 (0.9%) | 0.545 (0.5%) | [1.4, 0.8, 0.6] | D |
| Prog. 5 | 64:1 (40:1) | 0.56 (0.6%) | 0.030 (0.0%) | [1.4, 0.9, 0.6] | St |
| Prog. 6 | 22:1 (14:1) | 0.51 (0.6%) | 0.427 (0.4%) | [2.2, 1.8, 1.7] | M |
| Other prog. | 1.30 (1.4%) | 0.360 (0.3%) | [3.1, 1.4, 0.7] | ||
| Halo 27 | |||||
| Progenitor | Merger ratio | M⋆(< R200) [109 M⊙] | M⋆(Rhelio < 2.5 kpc) [107 M⊙] | zacc,5–50–90 | State |
| Total | 102.49 | 172.826 | |||
| In situ | 87.12 (85.0%) | 165.019 (95.5%) | |||
| Prog. 1 | 9:1 (4:1) | 5.39 (5.3%) | 2.949 (1.7%) | [1.4, 1.4, 1.3] | M |
| Prog. 2 | 9:1 (4:1) | 2.68 (2.6%) | 1.493 (0.9%) | [1.8, 1.7, 1.7] | M |
| Prog. 3 | 55:1 (8:1) | 2.10 (2.0%) | 2.680 (1.6%) | [1.8, 1.2, 1.0] | D |
| Prog. 4* | 28:1 (56:1) | 1.82 (1.8%) | 0.047 (0.0%) | [0.6, 0.3, 0.2] | St |
| Prog. 5 | 44:1 (4:1) | 0.78 (0.8%) | 0.191 (0.1%) | [2.4, 2.2, 2.2] | M |
| Prog. 6 | 53:1 (86:1) | 0.59 (0.6%) | 0.019 (0.0%) | [0.8, 0.8, 0.6] | M |
| Other prog. | 2.02 (2.0%) | 0.429 (0.2%) | [3.5, 2.2, 0.2] | ||
Notes. All the less massive progenitors are regrouped together under the label"Other prog.". Col. 2 indicates the ration between the total mass of the progenitor and the host galaxy at infall time, and the value in parentheses corresponds to the ratio between the stellar mass of the progenitor and the host. Col. 3 shows the stellar mass of each progenitor/in situ component in the entire volume of the galaxy (<R200). Col. 4 shows their stellar mass contribution in a sphere of 2.5 kpc radius around the Sun (solar vicinity). In these columns, the percentage of the stellar contribution of each progenitor relative to the total stellar mass in the respective volume is provided in parentheses. Col. 5 indicates the redshifts when 5, 50, and 90% of the particles of a given progenitor escaped its gravitational attraction and became bound to the main galaxy. Col. 6 indicated if after a visual inspection, the spatial distribution of the debris of an accreted galaxy present a stream-like (St) or a disc-like (D) structure, or if they do not display any particular shape and are then fully spatially mixed (M). Note that we indicate here only the stellar mass of the star particles of each progenitor flagged as accreted (ACCRETEDFLAG== 0). This does not take into account the mass of the stellar particles that are still bound to the satellite galaxy. The asterisk after the progenitor id indicate that more than 1% of the stellar mass of the accreted galaxy are still bound to the surviving progenitor. Moreover, the mass of each progenitor in the solar vicinity (Col. 3) correspond to the average mass in the solar vicinity of the four azimuths used to make the mocks.
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