Table 1.
Definition of our sample.
| Name | Optical type | log L14 − 195 | Hubble stage | Axis ratio | Distance | Redshift |
|---|---|---|---|---|---|---|
| [erg s−1] | [Mpc] | |||||
| NGC 2110 | Sy 2 (1h) | 43.64 | −3.0 | 0.74 | 34 | 0.007789 |
| NGC 2992 | Sy 1.8 | 42.62 | 1.0 | 0.3 | 36 | 0.00771 |
| MCG-05-23-016 | Sy 1.9 | 43.47 | −1.0 | 0.45 | 35 | 0.008486 |
| NGC 3081 | Sy 2 (1h) | 43.06 | 0.0 | 0.77 | 34 | 0.007976 |
| ESO 021-G004 | Sy 2 | 42.49 | −0.4 | 0.45 | 39 | 0.009841 |
| NGC 5728 | Sy 2 | 43.21 | 1.0 | 0.57 | 39 | 0.009353 |
| ESO 137-G034 | Sy 2 | 42.62 | 0.0 | 0.79 | 35 | 0.009144 |
| NGC 7172 | Sy 2 (1i) | 43.45 | 1.4 | 0.56 | 37 | 0.008683 |
| NGC 7582 | Sy 2 (1i) | 42.67 | 2.0 | 0.42 | 22 | 0.005254 |
| NGC 718 | inactive | – | 1.0 | 0.87 | 23 | 0.005781 |
| NGC 1079 | inactive | – | 0.0 | 0.6 | 19 | 0.004843 |
| NGC 1315 | inactive | – | −1.0 | 0.89 | 21 | 0.005387 |
| NGC 1947 | inactive | – | −3.0 | 0.87 | 19 | 0.003669 |
| ESO 208-G021 | inactive | – | −3.0 | 0.7 | 17 | 0.003619 |
| NGC 2775 | inactive | – | 2.0 | 0.77 | 21 | 0.004503 |
| NGC 3175 | inactive | – | 1.0 | 0.26 | 14 | 0.003673 |
| NGC 3351 | inactive | – | 3.0 | 0.93 | 11 | 0.002595 |
| ESO 093-G003 | inactive | – | 0.3 | 0.6 | 22 | 0.006106 |
| NGC 3717 | inactive | – | 3.0 | 0.18 | 24 | 0.005781 |
| NGC 3749 | inactive | – | 1.0 | 0.25 | 42 | 0.009013 |
| NGC 4224 | inactive | – | 1.0 | 0.35 | 41 | 0.008683 |
| NGC 4254 | inactive | – | 5.0 | 0.87 | 15 | 0.008029 |
| NGC 5037 | inactive | – | 1.0 | 0.32 | 35 | 0.006351 |
| NGC 5845 | inactive | – | −4.6 | 0.63 | 25 | 0.00491 |
| NGC 5921 | inactive | – | 4.0 | 0.82 | 21 | 0.004937 |
| IC 4653 | inactive | – | −0.5 | 0.63 | 26 | 0.00517 |
| NGC 7727 | inactive | – | 1.0 | 0.74 | 26 | 0.006231 |
Notes. Columns are: name, optical spectral type, observed 14–195 keV luminosity, Hubble stage, axis ratio, distance, and redshift from NED. Hard X-ray fluxes are from Swift/BAT (Baumgartner et al. 2013). For references and discussion on the latter four columns, see Davies et al. (2015). The optical spectral type is from our own analysis and follows the classification scheme of Véron-Cetty & Véron (2010).
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