Table 3
Black hole mass estimates from different relations.
| Used relation | log (MBH/M⊙) |
|
|
|
| broad line width | |
| A. Schulze (priv. comm.) | 7.4 |
| J. Scharwächter (priv. comm.) | 7.3 |
| Kim et al. (2010) | 7.3 |
| MBH − σ∗ relation | |
| Gültekin et al. (2009) | 7.0 (+0.5a) |
| Graham et al. (2011) | 6.7b (+0.5a>) |
| Kormendy & Ho (2013) | 7.4 (+0.5a) |
| MBH − Lbulge relationc | |
| Marconi & Hunt (2003) | 8.0 |
| Vika et al. (2012) | 8.2 |
| Graham & Scott (2013) | 8.4 |
| Kormendy & Ho (2013) | 8.4 |
| MBH − Mbulge relation | |
| Häring & Rix (2004) | 6.0–6.8 |
| Sani et al. (2011) | 6.6–7.1 |
| Scott et al. (2013) | 5.1–6.6/6.9–7.5d |
| Kormendy & Ho (2013) | 6.4–7.2 |
Notes. Note that the derivation of uncertainties for black hole masses is complex since it includes measurement uncertainties (e.g. of the flux measurement) but also the intrinsic scatter of the relations. Usually, the uncertainty will be at least 0.5 dex.
Correction for the difference between NIR (σCO) and optical (σopt) stellar velocity dispersion according to Riffel et al. (2015).
Note that the MBH − Lbulge relation is not a good estimator for active galaxies according to Busch et al. (2014).
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