Table 7.
BH masses from literature, and our derived ones.
| Galaxy | log MBH | log MBH | Ref. | log MBH | log LAGN |
|---|---|---|---|---|---|
| M⊙ | M⊙ | M⊙ | erg s−1 | ||
| (1) | (2) | (3) | (4) | (5) | (6) |
| N 613 | 6.87±.27 | 7.60±.35 | (1) | 7.57±.15 | 42.1 |
| N1326 | 7.47±.17 | 7.11±.33 | (2) | 6.81±.2 | 40.7 |
| N1365 | 6.05±.39 | 6.30±.4 | (3) | 6.60±.3 | 42.8 |
| N1433 | 6.61±.37 | 7.24±.4 | (4) | – | 40.0 |
| N1566 | 7.11±.32 | 6.48±.2 | (5) | 6.83±.3 | 41.4 |
| N1672 | 7.08±.9 | 6.00±.6 | (6) | 7.70±.1 | 39.3 |
| N1808 | 6.74±.35 | 7.20±.6 | (7) | – | 40.6 |
| N1068 | 6.93±.37 | 7.15±.1 | (8) | 7.17±.2 | 44.7 |
Notes. Column 2 lists BH masses estimated from the spiral pitch angle (Davis et al. 2014), except for NGC 1326, from the Sersic index (Mutlu-Pakdil et al. 2016). Column 3 is from other estimations: (1) van den Bosch (2016), (2) Mould et al. (2012), (3) Risaliti et al. (2009), (4) Smajić et al. (2014), (5) Smajić et al. (2015), (6) Jenkins et al. (2011), (7) Busch et al. (2017), (8) Gallimore et al. (2001). Column 5 displays our best fit estimates from the molecular gas dynamics. For NGC 1068, the value comes from the H2O masers (e.g., Lodato & Bertin 2003; Gallimore et al. 2016). Column 6 is the bolometric AGN luminosity (see Sect. 4.4.3).
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