Table 1
The 23 Large Program and archive targets included in this paper.
Name | RA | Dec | Type | Type | D | z | Scale | Coudé star | n (u,v) | Ref. | ||
[h m s] | [°′′′] | (1) | (2) | [Mpc] | [mas/pc] | Ψ[′′] | V [mag] | |||||
|
||||||||||||
1 | I Zw 1 | 00 53 35.1 | +12 41 34 | NL Sy 1 | Sy 1 | 222 | 0.0589 | 0.9 | 0 | 14.0 | 10 | 12 |
2 | NGC 424 | 01 11 27.6 | −38 05 00 | Sy 1h | Sy 2 | 44.7 | 0.0110 | 4.6 | 0 | 14.1 | 38 | 11 |
3 | NGC 1068 | 02 42 40.7 | −00 00 48 | Sy 1h | Sy 2 | 14.4 | 0.0038 | 14.3 | 0 | 10.8 | 32 | 0, 5, 12 |
4 | NGC 1365 | 03 33 36.4 | −36 08 25 | Sy 1.8 | Sy 1 | 18.1 | 0.0055 | 11.4 | 0 | 12.9 | 19 | 6, 12 |
5 | IRAS 05189−2524 | 05 21 01.7 | −25 21 45 | Sy 1h | Sy 2 | 167 | 0.0426 | 1.2 | 0 | 14.8 | 7 | 12 |
6 | H 0557−385 | 05 58 02.1 | −38 20 04 | Sy 1.2 | Sy 1 | 135 | 0.0339 | 1.5 | 0 | 15.0 | 4 | 10 |
7 | IRAS 09149−6206 | 09 16 09.4 | −62 19 30 | Sy 1 | Sy 1 | 222 | 0.0579 | 0.9 | 0 | 13.6 | 5 | 10 |
8 | MCG−05−23−16 | 09 47 40.2 | −30 56 54 | Sy 1i | Sy 2 | 38.8 | 0.0085 | 5.3 | 11 | 13.5 | 18 | 6, 9, 12 |
9 | Mrk 1239 | 09 52 19.1 | −01 36 43 | NL Sy 1 | Sy 1 | 84.5 | 0.0200 | 2.4 | 0 | 14.4 | 8 | 6, 9, 12 |
10 | NGC 3281 | 10 31 52.1 | −34 51 13 | Sy 2 | Sy 2 | 47.6 | 0.0107 | 4.3 | 15 | 15.7 | 7 | 12 |
11 | NGC 3783 | 11 39 01.8 | −37 44 19 | Sy 1.5 | Sy 1 | 43.8 | 0.0097 | 4.7 | 0 | 13.4 | 12 | 3, 4, 10 |
12 | NGC 4151 | 12 10 32.6 | +39 24 21 | Sy 1.5 | Sy 1 | 16.9 | 0.0033 | 12.2 | 0 | 11.8 | 14 | 7, 9, 10 |
13 | 3C 273 | 12 29 06.7 | +02 03 08 | Sy 1.0 | Quasar | 546 | 0.1580 | 0.4 | 0 | 12.8 | 3 | 6, 12 |
14 | NGC 4507 | 12 35 36.6 | −39 54 33 | Sy 1h | Sy 2 | 51.7 | 0.0118 | 4.0 | 28 | 16.0 | 10 | 6, 12 |
15 | NGC 4593 | 12 39 39.4 | −05 20 39 | Sy 1.0 | Sy 1 | 41.2 | 0.0090 | 5.0 | 0 | 13.2 | 9 | 12 |
16 | ESO 323−77 | 13 06 26.1 | −40 24 52 | Sy 1.2 | Sy 1 | 64.2 | 0.0150 | 3.2 | 0 | 13.4 | 9 | 10 |
17 | Centaurus A | 13 25 26.6 | −43 01 09 | ? | Sy 2 | 3.8 | 0.0018 | 54.3 | 45 | 12.5 | 12 | 1, 8 |
18 | IRAS 13349+2438 | 13 37 18.7 | +24 23 03 | NL Sy 1 | Sy 1 | 393 | 0.1076 | 0.5 | 0 | 15.0 | 6 | 10 |
19 | IC 4329 A | 13 49 19.3 | −30 18 34 | Sy 1.2 | Sy 1 | 68.3 | 0.0161 | 3.0 | 0 | 13.7 | 11 | 6, 9, 12 |
20 | Circinus | 14 13 09.9 | −65 20 21 | Sy 1h | Sy 2 | 4.2 | 0.0014 | 49.1 | 50 | 12.5 | 28 | 2 |
21 | NGC 5506 | 14 13 15.0 | −03 12 27 | Sy 1i | Sy 2 | 28.7 | 0.0062 | 7.2 | 0 | 14.4 | 12 | 6, 12 |
22 | NGC 5995 | 15 48 25.0 | −13 45 28 | Sy 1.9 | Sy 2 | 102 | 0.0252 | 2.0 | 0 | 13.7 | 4 | 12 |
23 | NGC 7469 | 23 03 15.6 | +08 52 26 | Sy 1.5 | Sy 1 | 60.9 | 0.0163 | 3.4 | 0 | 13.0 | 13 | 6, 12 |
|
||||||||||||
NGC 3227 | 10 23 30.6 | +19 51 54 | Sy 2 | Sy 2 | 20.2 | 0.0039 | 10.2 | 0 | 11.8 | 0 | 12 | |
IC 3639 | 12 40 52.8 | −36 45 21 | Sy 1h | Sy 2 | 48.3 | 0.0109 | 4.3 | 37 | 14.0 | 0 | 12 |
Notes. In addition the two sources for which only upper limits have been derived are included in this table. RA, Dec: J2000 coordinates. Type: (1) AGN type as classified by Véron-Cetty & Véron (2010): the classification of intermediate Seyfert types (1 < type < 2) is defined by the ratio of Hβ to [OIII]λ5007 fluxes. Sy 1h are “hidden” Seyfert 1 galaxies (i.e. where broad lines have been detected in polarized light), In the Sy 1i type, broad Pa β lines are detected “indicating the presence of a highly reddened broad line region”; (2) AGN type from SIMBAD. D: angular-size distance derived from redshift using the CMB reference frame and a concordance ΛCDM cosmology (plain typeface); redshift-independent distance measurement/average over several observations, see NED (italic typeface). z: redshift (from NED). Ψ: Coudé (MACAO) guide star separation from science target (0: guiding on nucleus). V[mag]: V magnitude of guide star; from Véron-Cetty & Véron (2010) if guide star is AGN. n(u,v) number of good fringe tracks at unique (u,v) positions (see text for explanation).
Reference. 0: Jaffe et al. (2004); 1: Meisenheimer et al. (2007); 2: Tristram et al. (2007); 3: Beckert et al. (2008); 4: Kishimoto et al. (2009); 5: Raban et al. (2009); 6: Tristram et al. (2009); 7: Burtscher et al. (2009); 8: Burtscher et al. (2010); 9: Tristram & Schartmann (2011); 10: Kishimoto et al. (2011b); 11: Hönig et al. (2012); 12: this work.
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