Table 2.
Parameters of quasars and absorption line systems.
| SDSS name | zem | zabs | υr | R | Cf | Log L3000 | Log MBH | η | ṀBH | RBELR | Rtorus | RNELR |
 |
 |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (km s−1) | (erg s−1) | (M⊙) | (M⊙ yr−1) | (pc) | (pc) | (pc) | (pc) | (pc) | ||||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13) | (14) | (15) |
| 004039.79+150321.2 | 0.8857 | 0.8929 | −1148 | 753 | 0.52 | 45.33 | 9.06 | −1.131 | 1.96 | 0.126 | 1.595 | 493.30 | 12.46 | 7.53 |
| 021144.19-063726.8 | 1.0205 | 1.0278 | −1081 | – | 0.53 | 45.16 | 8.84 | −1.081 | 1.31 | 0.144 | 1.304 | 376.59 | 7.26 | 5.06 |
| 111537.58+121845.2 | 1.1790 | 1.1868 | −1073 | – | 0.60 | 45.79 | 9.08 | −0.698 | 5.53 | 0.219 | 2.682 | 990.42 | 16.05 | 8.99 |
| 113716.69+124645.4 | 1.4898 | 1.5063 | −1979 | 5703 | 0.81 | 45.19 | 8.95 | −1.170 | 1.37 | 0.104 | 1.333 | 388.21 | 1.48 | 1.94 |
| 114229.33+455728.9 | 1.0904 | 1.0979 | −1071 | 546 | 0.84 | 44.85 | 8.81 | −1.367 | 0.64 | 0.069 | 0.909 | 232.25 | 6.67 | 4.83 |
| 124055.64+571853.9 | 1.2489 | 1.2570 | −1080 | 79 | 0.82 | 45.43 | 8.89 | −0.862 | 2.46 | 0.142 | 1.788 | 575.15 | 8.04 | 5.76 |
| 143717.59+390844.8 | 0.7086 | 0.7149 | −1099 | – | 0.93 | 44.60 | 8.33 | −1.129 | 0.36 | 0.054 | 0.684 | 158.76 | 1.70 | 1.50 |
| 150805.22+140845.4 | 0.9170 | 0.9252 | −1286 | 7717 | 0.77 | 45.42 | 8.70 | −0.689 | 2.37 | 0.140 | 1.755 | 560.78 | 2.78 | 2.62 |
| 212523.78-015124.8 | 0.8808 | 0.8885 | −1227 | – | 0.83 | 44.57 | 8.28 | −1.123 | 0.34 | 0.042 | 0.662 | 151.97 | 1.04 | 1.09 |
Note. Column (4): Relative velocities of absorbers with respect to quasar emission line redshifts; (5) 
, which represents the radio loudness of quasars; (6) The coverage fraction of the Mg II absorbing cloud relative to the continuum emission region; (7) The monochromatic luminosity of the quasar at 3000 Å; (8) The mass of the black hole; (9) The Eddingtion ratio η = Lbol/LEdd; (10) The mass accretion rate of the black hole; (11) The size of the broad emission line region; (12) The inner radius of dusty torus; (13) The size of the narrow emission line region; (14) The largest distances of absorbers from the central SMBH, considering the gravitational potential contributed by the central SMBH and a Hernquist stellar distribution for the hosting galaxy (Hernquist 1990); (15) The largest distances of absorbers from the central SMBH, only considering the gravitational field of the latter.
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