Table 1.
Values of 
and the associated probability of belonging to the distribution of single MBHs for single and (mock) binary MBH.
| Name |
 |
P | “Solidity” |
|---|---|---|---|
| Mrk 142 | 0.73 | 0.04 | |
| SBS 1116+583A | 0.77 | 0.2 | |
| Arp 151 | 0.97 | > 0.99 | |
| Mrk 1310 | 0.89 | > 0.99 | |
| Mrk 202 | 0.84 | 0.71 | |
| NGC 4253 | 0.74 | 0.06 | |
| NGC 4748 | 0.83 | 0.64 | |
| NGC 5548 | 0.74 | 0.06 | |
| NGC 6814 | 0.88 | 0.97 | |
| Mrk 142_50 | 0.66 | < 10−3 | |
| Mrk 142_100 | 0.71 | 0.01 | |
| Mrk 142_300 | 0.78 | 0.26 | Solid |
| Mrk 142_1000 | 0.81 | 0.49 | Solid |
| SBS 1116+583A_50 | 0.38 | < 10−3 | |
| SBS 1116+583A_100 | 0.37 | < 10−3 | |
| SBS 1116+583A_300 | 0.41 | < 10−3 | Solid |
| SBS 1116+583A_1000 | 0.45 | < 10−3 | Solid |
| Arp 151_50 | –0.42 | < 10−3 | |
| Arp 151_100 | –0.29 | < 10−3 | |
| Arp 151_300 | –0.09 | < 10−3 | Solid |
| Arp 151_1000 | 0.14 | < 10−3 | Solid |
| Mrk 1310_50 | 0.05 | < 10−3 | |
| Mrk 1310_100 | 0.12 | < 10−3 | |
| Mrk 1310_300 | 0.24 | < 10−3 | Solid |
| Mrk 1310_1000 | 0.41 | < 10−3 | Solid |
| Mrk 202_50 | 0.5 | < 10−3 | |
| Mrk 202_100 | 0.53 | < 10−3 | |
| Mrk 202_300 | 0.62 | < 10−3 | Solid |
| Mrk 202_1000 | 0.71 | 0.01 | Solid |
| NGC 4253_50 | 0.3 | < 10−3 | |
| NGC 4253_100 | 0.37 | < 10−3 | |
| NGC 4253_300 | 0.36 | < 10−3 | Solid |
| NGC 4253_1000 | 0.5 | < 10−3 | Solid |
| NGC 4748_50 | –0.16 | < 10−3 | |
| NGC 4748_100 | –0.1 | < 10−3 | |
| NGC 4748_300 | 0.11 | < 10−3 | Solid |
| NGC 4748_1000 | 0.31 | < 10−3 | Solid |
| NGC 5548_50 | 0.69 | 0.004 | |
| NGC 5548_100 | 0.7 | 0.008 | |
| NGC 5548_300 | 0.8 | 0.4 | Solid |
| NGC 5548_1000 | 0.88 | 0.97 | Solid |
| NGC 6814_50 | 0.8 | 0.41 | |
| NGC 6814_100 | 0.82 | 0.56 | |
| NGC 6814_300 | 0.9 | > 0.99 | Solid |
| NGC 6814_1000 | 0.9 | > 0.99 | Solid |
Notes. The values of 
are restricted to the bulk of the line, while the associated probability of belonging to the distribution of single MBHs have been calculated using the median cumulative distribution for 
shown with the solid line in Fig. 6. The names of the mocks are constructed by attaching the period of the binary (in yr) to the name of the real AGN progenitor. The last column identifies the “solid” binaries, for which a stable disc-like BLR can exist around both MBHs. Considering that our inferred cumulative distribution for the 
is well determined up to probabilities of as low as ∼103, we consider smaller values as upper limits.
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