Table 1.
Main properties of the sample used in this paper.
| Name | α2000(a) | δ2000(a) | Dist (b) | Hubble type (b) | AGN type (b) | PAphot(c) | iphot(c) | log10L14 − 150 keV(d) | log10L2 − 10 keV(d) | log (e) |
log10N(H)Xabs(d) |
|---|---|---|---|---|---|---|---|---|---|---|---|
| hms | ° ′ ″ | Mpc | – | – | ° | ° | erg s−1 | erg s−1 | – | cm−2 | |
| NGC 6300 | 17:16:59.473 | −62:49:13.98 | 14.0 | SB(rs)b | Sy2 | 120 | 53 | 42.3 | 41.7 | −1.9 | 23.3 |
| NGC 5643 | 14:32:40.778 | −44:10:28.60 | 16.9 | SAB(rs)c | Sy2 | 98 | 30 | 43.0 | 42.4 | −1.3 | 25.4 |
| NGC 7314 | 22:35:46.230 | −26:03:00.90 | 17.4 | SAB(rs)bc | Sy1.9, S1h | 3 | 70 | 42.2 | 42.2 | −1.2 | 21.6 |
| NGC 4388 | 12:25:46.820 | +12:39:43.45 | 18.1 | SA(s)b | Sy1.9, S1h | 91 | 90 | 43.0 | 42.5 | −1.1 | 23.5 |
| NGC 4941 | 13:04:13.143 | −05:33:05.83 | 20.5 | (R)SAB(r)ab | Sy2 | 22 | 37 | 42.0 | 41.4 | −2.4 | 23.7 |
| NGC 7213 | 22:09:16.260 | −47:09:59.95 | 22.0 | SA(s)a | Sy1.5, radio-source | 124 | 39 | 42.3 | 41.9 | −3.0 | 20.0 |
| NGC 7582 | 23:18:23.621 | −42:22:14.06 | 22.5 | (R’)SB(s)ab | Sy2, S1i | 156 | 68 | 43.2 | 43.5 | −1.7 | 24.3 |
| NGC 6814 | 19:42:40.576 | −10:19:25.50 | 22.8 | SAB(rs)bc | Sy1.5 | 108 | 52 | 42.6 | 42.2 | −1.6 | 21.0 |
| NGC 5506 | 14:13:14.901 | −03:12:27.22 | 26.4 | Sa peculiar | Sy1.9, S1i | 89 | 90 | 43.2 | 43.0 | −2.3 | 22.4 |
| NGC 7465 | 23:02:00.952 | +15:57:53.55 | 27.2 | (R’)SB(s)0 | Sy2, S3 | 162 | 64 | 42.0 | 41.9 | −2.2 | 21.5 |
| NGC 1068 | 02:42:40.771 | −00:00:47.84 | 14.0 | (R)SA(rs)b | Sy2 | 73 | 35 | 42.7 | 42.8 | −0.3 | 25.0 |
| NGC 1365 | 03:33:36.458 | −36:08:26.37 | 18.3 | (R’)SBb(s)b | S1.8 | 23 | 63 | 42.3 | 42.1 | −2.8 | 22.2 |
| NGC 3227 | 10:23:30.570 | +19:51:54.30 | 23.0 | SAB(s)a pec | S1.5 | 156 | 68 | 42.8 | 42.4 | −1.2 | 21.0 |
Notes.
Phase tracking centers of the band 7 ALMA observations used in this work, which cover the GATOS core sample of ten galaxies, listed first, and three additional targets from the literature: NGC 1068 (García-Burillo et al. 2019), NGC 1365 (Combes et al. 2019), and NGC 3227 (Alonso-Herrero et al. 2019).
Distances are median values of redshift-independent estimates from the Nasa Extragalactic Database (NED) after excluding select measurements from unreliable or outdated references; Hubble and AGN type taken from NED. In addition to the standard classification as a function of AGN class (1, 2, and intermediate types: 1.n, where n ranges from 5 to 9 and numerically larger subclasses have weaker broad-line components relative to the narrow lines, following the notation of Osterbrock 1981), some objects are classified as S1h or S1i if broad polarized Balmer lines or broad Paschen lines in the infrared are detected, respectively, according to the nomenclature of Véron-Cetty & Véron (2006).
Position angle (PAphot) and inclination (iphot) of the optical disks based on photometric estimates taken from HyperLeda (http://leda.univ-lyon1.fr/).
Luminosities of hard X-rays (L14 − 150 keV and L2 − 10 keV) and gas column densities of obscuring material (N(H)Xabs) are taken from Ricci et al. (2017a); L14 − 150 keV and L2 − 10 keV are intrinsic luminosities (corrected for absorption) and re-scaled to the adopted distances.
Eddington ratios (
) taken from Koss et al. (2017).
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