Table 1.
Merger parameters.
| # merger | z | MBH [M⊙] | Mb [M⊙] | Mh [M⊙] | e | rp [kpc] |
|---|---|---|---|---|---|---|
| ID merger tree = 17187 | ||||||
| I | 1.90 | 4.23e+08 | 9.89e+10 | 2.75e+12 | 0.99 | 2.71e-01 |
| 2.19e+08 | 4.09e+10 | 3.84e+10 | ||||
| II | 0.21 | 7.29e+08 | 5.34e+11 | 1.29e+14 | 0.39 | 3.70e+01 |
| 7.21e+08 | 1.27e+11 | 2.87e+11 | ||||
| III | 0.17 | (7.29+7.21)e+08 | (5.34+1.27)e+11 | (1.29+2.87)e+14 | 0.89 | 3.64 |
| 7.30e+08 | 8.94e+10 | 1.24e+11 | ||||
| ID merger tree = 125027 | ||||||
| I | 2.00 | 4.64e+08 | 9.57e+10 | 3.85e+12 | 0.985 | 9.17e-02 |
| 1.26e+08 | 2.51e+10 | 1.06e+10 | ||||
| II | 1.60 | 5.97e+08 | 1.41e+11 | 6.75e+12 | 0.97 | 1.32 |
| 3.32e+08 | 3.91e+10 | 1.59e+11 | ||||
| ID merger tree = 125028 | ||||||
| I | 1.60 | 3.16e+08 | 6.63e+10 | 3.15e+11 | 0.98 | 1.09 |
| 3.55e+08 | 7.73e+10 | 4.71e+12 | ||||
| II | 1.41 | (3.16+3.55)e+08 | (6.63+7.73)e+10 | (0.315+4.71)e+12 | 0.85 | 7.63e-01 |
| 3.55e+08 | 3.22e+10 | 7.25e+09 | ||||
| III | 0.92 | 6.91e+08 | 3.16e+11 | 1.29e+13 | 0.987 | 2.99e-01 |
| 6.49e+08 | 1.06e+11 | 6.93e+10 | ||||
| ID merger tree = 168390 | ||||||
| I | 1.41 | 3.31e+08 | 4.74e+10 | 4.17e+10 | 0.775 | 9.26 |
| 2.22e+08 | 7.44e+10 | 5.71e+12 | ||||
| II | 1.30 | (3.31+2.22)e+08 | (4.74+7.44)e+10 | (0.04+5.71)e+12 | 0.947 | 3.23e-01 |
| 3.26e+08 | 3.53e+10 | 7.66e+09 | ||||
| ID merger tree = 197109 | ||||||
| I | 2.00 | 2.49e+07 | 1.998e+10 | 1.07e+12 | 0.745 | 2.25 |
| 2.26e+07 | 5.24e+09 | 6.75e+09 | ||||
| II | 1.36 | 1.27e+08 | 6.61e+10 | 2.50e+12 | 0.986 | 2.35e-01 |
| 1.25e+08 | 2.68e+10 | 3.39e+10 | ||||
| III | 1.30 | (1.27+1.25)e+08 | (6.61+2.68)e+10 | (0.03+2.50)e+12 | 0.997 | 2.22e-01 |
| 1.46e+08 | 1.78e+10 | 3.46e+09 | ||||
Notes. Parameters related to the mergers in the five merger trees: z is the initial redshift; MBH, Mb, and Mh denote the mass of the BH, the stellar bulge, and the DM halo, respectively, as reported in TNG100-1. Each box contains data corresponding to the primary (top row) and secondary galaxy (bottom row). When a subsequent merger occurs before the previous merger’s remnant has time to form, we report the masses of the primary components (BH, bulge, and halo) as the sum of the elements of the previous merger. Finally, e and rp are the eccentricity of each merger’s orbit and its pericentre distance, computed following the method outlined in Sect. 2.3 of Fastidio et al. (2024).
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