The sources in our sample. Luminosity distance, DL, BH mass, MBH, the Eddington ratio (λEdd), the photon index (Γ), and the 2–10 keV luminosity obtained from the X-ray spectral analysis (see text for details).
| Source . | |$D_{\rm L}^{^a}$| . | |$M_{\rm BH}^{^{b}}$| . | |$\lambda _{\rm Edd}^{^{c}}$| . | Γ . | |$L_{\rm 2\!-\!10}^{^d}$| . |
|---|---|---|---|---|---|
| . | (Mpc) . | |$(10^7\, M_\odot$|) . | . | . | (|$10^{43}\, \rm cgs$|) . |
| NGC 4593 | 38.8 | |$0.76^{+ 0.16}_{-0.16}$| | 0.08 | 1.74 | 0.6 ± 0.2 |
| NGC 5548 | 80.1 | |$7.0 ^{+2.0}_{-2.8}$| | 0.05 | 1.70 | 2.5 ± 0.7 |
| Fairall 9 | 209 | |$19.9_{-4.6}^{+3.9}$| | 0.03 | 1.90 | 9.7 ± 1.9 |
| Mrk 817 | 138.7 | |$3.8^{+0.6}_{-0.6}$| | 0.20 | 1.90 | 1.9 ± 1.3 |
| Source . | |$D_{\rm L}^{^a}$| . | |$M_{\rm BH}^{^{b}}$| . | |$\lambda _{\rm Edd}^{^{c}}$| . | Γ . | |$L_{\rm 2\!-\!10}^{^d}$| . |
|---|---|---|---|---|---|
| . | (Mpc) . | |$(10^7\, M_\odot$|) . | . | . | (|$10^{43}\, \rm cgs$|) . |
| NGC 4593 | 38.8 | |$0.76^{+ 0.16}_{-0.16}$| | 0.08 | 1.74 | 0.6 ± 0.2 |
| NGC 5548 | 80.1 | |$7.0 ^{+2.0}_{-2.8}$| | 0.05 | 1.70 | 2.5 ± 0.7 |
| Fairall 9 | 209 | |$19.9_{-4.6}^{+3.9}$| | 0.03 | 1.90 | 9.7 ± 1.9 |
| Mrk 817 | 138.7 | |$3.8^{+0.6}_{-0.6}$| | 0.20 | 1.90 | 1.9 ± 1.3 |
aWe computed DL using the source redshift, assuming a flat Universe with: |$H_0 = 67.8\, \rm km\, s^{-1}\, Mpc^{-1}$|, ΩΛ = 0.7, and ΩM = 0.3.
b MBH are from ‘The AGN Black Hole Mass Database’ (Bentz & Katz 2015) except for NGC 5548 we use the estimate by Horne et al. (2021); we use the estimates when considering all emission lines.
cReferences to the Eddington rations: Cackett et al. (2018) for NGC 4593, Fausnaugh et al. (2016) for NGC 5548, Vasudevan & Fabian (2007) for Fairall 9, and Kara et al. (2021) for Mrk 817.
dThe uncertainty on the 2–10 keV luminosity represent the scatter around the mean in the X-ray light curves of each of the sources.
The sources in our sample. Luminosity distance, DL, BH mass, MBH, the Eddington ratio (λEdd), the photon index (Γ), and the 2–10 keV luminosity obtained from the X-ray spectral analysis (see text for details).
| Source . | |$D_{\rm L}^{^a}$| . | |$M_{\rm BH}^{^{b}}$| . | |$\lambda _{\rm Edd}^{^{c}}$| . | Γ . | |$L_{\rm 2\!-\!10}^{^d}$| . |
|---|---|---|---|---|---|
| . | (Mpc) . | |$(10^7\, M_\odot$|) . | . | . | (|$10^{43}\, \rm cgs$|) . |
| NGC 4593 | 38.8 | |$0.76^{+ 0.16}_{-0.16}$| | 0.08 | 1.74 | 0.6 ± 0.2 |
| NGC 5548 | 80.1 | |$7.0 ^{+2.0}_{-2.8}$| | 0.05 | 1.70 | 2.5 ± 0.7 |
| Fairall 9 | 209 | |$19.9_{-4.6}^{+3.9}$| | 0.03 | 1.90 | 9.7 ± 1.9 |
| Mrk 817 | 138.7 | |$3.8^{+0.6}_{-0.6}$| | 0.20 | 1.90 | 1.9 ± 1.3 |
| Source . | |$D_{\rm L}^{^a}$| . | |$M_{\rm BH}^{^{b}}$| . | |$\lambda _{\rm Edd}^{^{c}}$| . | Γ . | |$L_{\rm 2\!-\!10}^{^d}$| . |
|---|---|---|---|---|---|
| . | (Mpc) . | |$(10^7\, M_\odot$|) . | . | . | (|$10^{43}\, \rm cgs$|) . |
| NGC 4593 | 38.8 | |$0.76^{+ 0.16}_{-0.16}$| | 0.08 | 1.74 | 0.6 ± 0.2 |
| NGC 5548 | 80.1 | |$7.0 ^{+2.0}_{-2.8}$| | 0.05 | 1.70 | 2.5 ± 0.7 |
| Fairall 9 | 209 | |$19.9_{-4.6}^{+3.9}$| | 0.03 | 1.90 | 9.7 ± 1.9 |
| Mrk 817 | 138.7 | |$3.8^{+0.6}_{-0.6}$| | 0.20 | 1.90 | 1.9 ± 1.3 |
aWe computed DL using the source redshift, assuming a flat Universe with: |$H_0 = 67.8\, \rm km\, s^{-1}\, Mpc^{-1}$|, ΩΛ = 0.7, and ΩM = 0.3.
b MBH are from ‘The AGN Black Hole Mass Database’ (Bentz & Katz 2015) except for NGC 5548 we use the estimate by Horne et al. (2021); we use the estimates when considering all emission lines.
cReferences to the Eddington rations: Cackett et al. (2018) for NGC 4593, Fausnaugh et al. (2016) for NGC 5548, Vasudevan & Fabian (2007) for Fairall 9, and Kara et al. (2021) for Mrk 817.
dThe uncertainty on the 2–10 keV luminosity represent the scatter around the mean in the X-ray light curves of each of the sources.
This PDF is available to Subscribers Only
View Article Abstract & Purchase OptionsFor full access to this pdf, sign in to an existing account, or purchase an annual subscription.
