Table A.1.
AGN distances and bolometric luminosities.
| Source | DL (Mpc) | log Lbol, 14−195 keV | log Lbol, 12 μm | log Lbol,5100 Å | log Lbol, use |
|---|---|---|---|---|---|
| NGC 1365 | 16.6 | 42.96 | 43.05 | ... | 42.96 |
| NGC 3783 | 47.8 | 44.52 | 44.27 | 44.27 | 44.52 |
| Mrk 335 | 113.6 | 44.19 | ... | 44.80 | 44.80 |
| 3C 120 | 144.9 | 45.28 | 44.90 | 44.01 | 45.28 |
| Mrk 509 | 149.4 | 45.31 | 44.91 | 45.11 | 45.31 |
| IRAS 09149−6206 | 254.7 | 45.29 | 45.64 | 45.72 | 45.29 |
| 3C 273 | 755.0 | ... | 46.44 | 46.64 | 46.64 |
| PDS 456 | 893.2 | ... | ... | 47.00 | 47.00 |
| NGC 4051 | 13.4 | 42.54 | 42.96 | 43.06 | 42.54 |
| NGC 4151 | 9.9 | 43.51 | 43.10 | 43.54 | 43.51 |
| Mrk 231 | 185.6 | ... | 45.82 | ... | 45.82 |
| IRAS 13349+2438 | 499.8 | ... | 46.26 | ... | 46.26 |
| Mrk 6 | 82.6 | 44.50 | ... | 44.80 | 44.50 |
| Ark 120 | 140.4 | 45.09 | 44.84 | 45.49 | 45.09 |
| IC 4329A | 69.4 | 45.10 | 44.83 | 44.19 | 45.10 |
| NGC 3227 | 18.8 | 43.36 | 42.92 | 43.45 | 43.36 |
| NGC 7469 | 69.4 | 44.38 | 44.47 | 44.69 | 44.38 |
| PG 1202+281 | 791.8 | ... | ... | 45.45 | 45.45 |
| Fairall 9 | 203.9 | 45.31 | 45.23 | 44.92 | 45.31 |
| Mrk 744 | 50.6 | 43.41 | ... | ... | 43.41 |
| NGC 5548 | 73.8 | 44.52 | 43.98 | 44.09 | 44.52 |
| Mrk 590 | 118.0 | 44.20 | 44.31 | 44.34 | 44.20 |
| MCG +08−11−011 | 87.0 | 44.95 | ... | 44.39 | 44.95 |
| Mrk 79 | 95.8 | 44.52 | ... | 44.49 | 44.52 |
| Mrk 110 | 158.4 | 45.12 | ... | 44.57 | 45.12 |
| NGC 3516 | 51.5 | 44.37 | ... | 44.05 | 44.37 |
| NGC 4593 | 34.7 | 43.86 | 43.53 | 43.92 | 43.86 |
| Mrk 817 | 138.2 | 44.60 | ... | 44.53 | 44.60 |
| IRAS 03450+0055 | 135.9 | ... | ... | 44.49 | 44.49 |
Notes. All luminosities are in units of erg s−1. (1) Source name. (2) Luminosity distance, calculated with H0 = 70 km s−1, ΩΛ = 0.7, and ΩM = 0.3. (3) Bolometric luminosity derived from 14–195 keV data. The X-ray data come from the BAT AGN Spectroscopic Survey (Baumgartner et al. 2013; Koss et al. 2017). (4) Bolometric luminosity derived from 12 μm data. The MIR data mainly come from Asmus et al. (2014), except for that of Mrk 231 (see Appendix A). (5) Bolometric luminosity derived from optical 5100 Å continuum data. The optical data mainly come from the BAT AGN catalog, except for those of PDS 456 and PG 1202+281 (see Appendix A). (6) The bolometric luminosity that we adopt for the R–L relation. The 14–195 keV bolometric luminosities are preferred, unless the objects are noted individually.
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