Table 3.
BH mass and Eddington ratio derived with dust continuum size.
| Name | log RBLR | log MBH | log λEdd |
|---|---|---|---|
| (ld) | (M⊙) | ||
| (1) | (2) | (3) | (4) |
| NGC 1365 | 0.57 ± 0.26 | 6.26 | −1.51 |
| IRAS 03450+0055 | 1.50 ± 0.25 | 7.77 | −1.02 |
| IRAS 09149−6206 | 1.67 ± 0.25 | 8.23 | −0.37 |
| Mrk 1239 | 1.27 ± 0.26 | 6.40 | 0.96 |
| WPVS 48 | 1.15 ± 0.25 | 6.99 | −0.54 |
| HE 1029−1401 | 1.93 ± 0.26 | 8.73 | −1.28 |
| Mrk 744 | 0.60 ± 0.25 | 7.39 | −2.73 |
| GQ Com | 1.62 ± 0.26 | 8.32 | −0.86 |
| Mrk 231 | 1.58 ± 0.27 | 7.87 | −0.01 |
| ESO 323-G77 | 0.99 ± 0.25 | 7.12 | −1.17 |
| IRAS 13349+2438 | 2.03 ± 0.25 | 7.83 | 0.02 |
| IC 4329A | 1.24 ± 0.25 | 8.17 | −2.10 |
| PGC 50427 | 0.97 ± 0.25 | 7.22 | −1.27 |
| PDS 456 | 2.19 ± 0.26 | 8.68 | 0.47 |
| PGC 89171 | 1.47 ± 0.26 | 7.61 | −0.85 |
| NGC 7603 | 1.51 ± 0.26 | 8.41 | −1.15 |
Notes. Column (1): Target name. Column (2): BLR radius derived from Rd with Eq. (4). However, we find the difference between the results using the best-fit relations with β fixed and free is much smaller than the uncertainties. Column (3): BH mass derived from RBLR and Hβ FWHM assuming the virial factor f = 1. Column (4): Eddington ratio derived from λLλ(5100 Å) (Col. (9) of Table 1) and BH mass from Col. (3).
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