Table B.2.
Estimates for black hole mass and Doppler factor in the EHT+ AGN sample
| Name | M• (108 M⊙) | Ref. | δ | Ref. | Name | M• (108 M⊙) | Ref. | δ | Ref. | |
|---|---|---|---|---|---|---|---|---|---|---|
| 3C 279 | 2.47 ± 0.26a | 1 | 23.8 | 7 | M 87 | 65.0 ± 2.0b | 2 | 1.0 | – | |
| OJ 287 | ∼1.0c | 3 | 16.8 | 7 | Cen A | 0.55 ± 0.30d | 4 | 1.0 | – | |
| J1924–2914 | 1 | – | 10.0 | – | NRAO 530 | ∼3.0e | 5 | 10.6 | 7 | |
| 3C 273 | 7.83 ± 2.50a | 1 | 16.8 | 7 | 1749+096 | 1 | – | 11.9 | 7 | |
| 1055+018 | 7.90 ± 0.36a | 1 | 12.1 | 7 | BL Lac | ∼1.7f | 6 | 7.2 | 7 | |
| 3C 84 | ∼3.0f | 6 | 6.9 | 8 | 3C 454.3 | 12.17 ± 2.38a | 1 | 32.9 | 8 | |
| CTA 102 | 6.39 ± 0.24a | 1 | 15.5 | 8 | J0132–1654 | 1 | – | 10.0 | – | |
| J0006–0623 | 1 | – | 5.1 | 7 | NGC 1052 | ∼1.55f | 6 | 0.3 | 7 |
Notes.
stellar velocity dispersion Doppler factors are estimated from 15 GHz variability (7 & refs. therein) or 43 GHz kinematics (8). If a source is not available in (7), the measurement is taken from (8). We assumed a Doppler factor δ = 1 for the remaining radio galaxies (M 87 and Cen A), and δ = 10 for the remaining quasars (J1924–2914 and J0006–0623).
References. (1) Torrealba (2012), Torrealba et al. (2012); (2) The Event Horizon Telescope Collaboration (2019a); (3) Komossa et al. (2023); (4) Neumayer (2010); (5) Keck (2019); (6) Woo & Urry (2002); (7) Pushkarev et al. (2017); (8) Weaver et al. (2022)
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