Table 1.
Properties of the sample.
| Galaxy | Type | Seyfert | Dist | 1″ | log L(2–10 keV) | Ref. |
|---|---|---|---|---|---|---|
| class | (Mpc) | (pc) | (erg s−1) | |||
| IC 4518W | Sc pec | 2 | 67.9 | 319 | 42.58 | 1 |
| Mrk 1066 | (R)SB0+(s) | 2 | 47.2 | 224 | 42.92 | 2 |
| NGC 1068 | (R)SA(rs)b | 2 | 14.0 | 67 | 42.80 | 1 |
| NGC 1320 | Sa? edge-on | 2 | 34.5 | 164 | 42.7–42.3 | 3 |
| NGC 1365 | SB(s)b | 1.8 | 18.3 | 102 | 42.09 | 1 |
| NGC 1386 | SB0+(s) | 1!‘ | 18.0 | 102 | 40.9–41.7 | 3 |
| NGC 1808 | (R)SAB(s)a | 2 | 14.0 | 67 | 40.40 | 3 |
| NGC 2110 | SAB0- | 1!‘ | 33.1 | 158 | 42.68 | 1 |
| NGC 2273 | SB(r)a? | 2 | 25.8 | 124 | 42.70 | 2 |
| NGC 2992 | Sa pec | 1!‘ | 36.6 | 174 | 42.09 | 1 |
| NGC 3081 | (R)SAB0/a(r) | 2 | 37.7 | 179 | 42.81 | 1 |
| NGC 3227 | SAB(s)a pec | 1.5 | 20.4 | 98 | 42.27 | 1 |
| NGC 4253 | (R’)SB(s)a? | 1.5 | 57.6 | 272 | 42.74 | 1 |
| NGC 4388 | SA(s)b? edge-on | 1.9 | 18.1 | 102 | 42.45 | 1 |
| NGC 5135 | SB(s)ab | 2 | 60.9 | 287 | 43.00 | 4 |
| NGC 5643 | SAB(rs)c | 2 | 19.2 | 92 | 42.53 | 1 |
| NGC 7130 | Sa pec | 2 | 63.6 | 299 | 42.05 | 1 |
| NGC 7172 | Sa pec edge-on | 2 | 32.1 | 153 | 42.62 | 1 |
| NGC 7213 | SA(s)a? | 1 | 21.2 | 102 | 41.81 | 1 |
| NGC 7465 | (R’)SB00?(s) | 2 | 21.9 | 105 | 41.74 | 1 |
| NGC 7469 | (R’)SAB(rs)a | 1.5 | 62.6 | 295 | 43.09 | 1 |
| NGC 7582 | (R’)SB(s)ab | 1!‘ | 18.3 | 88 | 43.31 | 1 |
Notes. Morphological types are from the Revised Catalog 3 (RC3) Catalogue (de Vaucouleurs et al. 1991). The Seyfert class is taken from Véron-Cetty & Véron (2006) except for NGC 1808, NGC 3081, and NGC 7213, which are taken from Veron-Cetty & Veron (1985), Phillips et al. (1983), and Phillips (1979), respectively. The “Sy1!‘” classification means that broad hydrogen recombination lines have been detected in the near-IR. Luminosity distances and angular scales are taken from the NASA/IPAC Extragalactic Database (NED) for H0 = 73 km s−1 Mpc−1, ΩM = 0.27 and ΩV = 0.30. NGC 1386 and NGC 1365 are in the Fornax Cluster. NGC 4388 is in the Virgo Cluster. The hard X-ray luminosities are intrinsic (i.e., corrected for absorption), and the last column indicates the reference.
References. 1. The BAT AGN Spectroscopic Survey (BASS) http://www.bass-survey.com/, Koss et al. (2017), Ricci et al. (2017), 2. Marinucci et al. (2012) 3. Brightman & Nandra (2011), 4. Pereira-Santaella et al. (2011).
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