Table 4
Results from the fit of four blazars.
| Source name | νp |  |
M0.9 | M0.9982 | Ṁ0.9 | Ṁ0.9982 | ℓEdd,0.9 | ℓEdd,0.9982 |
|---|---|---|---|---|---|---|---|---|
| [1] | [2] | [3] | [4] | [5] | [6] | [7] | [8] | [9] |
| S5 0014+813 | 15.33 | 47.92 | 10.04 | 10.14 | 153.3 | 106.4 | 0.99 | 1.12 |
| SDSS J013127.34-032100.1 | 15.21 | 47.34 | 9.99 | 10.09 | 40 | 27.8 | 0.29 | 0.33 |
| SDSS J074625.87+254902.1 | 15.38 | 46.31 | 9.15 | 9.25 | 3.8 | 2.6 | 0.19 | 0.21 |
| SDSS J161341.06+341247.8 | 15.22 | 46.46 | 9.53 | 9.64 | 5.3 | 3.7 | 0.11 | 0.12 |
Notes. Columns are: [1] name of the source; [2] Log of the spectrum peak frequency in units of Hz; [3] Log of the spectrum peak luminosity in units of erg s−1; [4,5] Log of the KERRBB BH mass related to a = 0.9 and a = 0.9982 in units of solar masses; [6,7] Log of the KERRBB accretion rate related to a = 0.9 and a = 0.9982 in units of M⊙ yr−1; [8,9] the Eddington ratio related to a = 0.9 and a = 0.9982. Following LN89, the Eddington ratio is above or near the limit of the thin disk reliability for only two sources (ℓEdd < 0.3 → Fig. 10).
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