Table 3.
Results from the analysis of the optical spectra.
| ID | Inst. | Comp. | [O I] |
 |
 |
 |
 |
 |
 |
fblend |
|---|---|---|---|---|---|---|---|---|---|---|
| (km s−1) | (km s−1) | (km s−1) | (km s−1) | (km s−1) | (km s−1) | (%) | ||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) |
| NGC 2685 | HST/STIS | N | N | 80 ± 1 | 63 ± 12 | – | – | – | – | – |
| Palomar | N | Y | –10 ± 1 | 70 ± 10 | – | – | – | – | – | |
| NGC 3245 | HST/STIS | N + B | N | 134 ± 29 | 172 ± 6 | – | – | 424 ± 12 | 998 ± 6 | 47 |
| Palomar | N + S | Y | –216 ± 9 | 25 ± 40 | 94 ± 17 | 136 ± 21 | − | − | − | |
| NGC 4374 | HST/STIS | N + S + B | Y | −275 ± 13 | 146 ± 14 | 362 ± 5 | 281 ± 24 | 693 ± 7 | 1432 ± 37 | 65 |
| Palomar | N + S | Y | 117 ± 4 | 51 ± 29 | 33 ± 56 | 395 ± 71 | − | − | − | |
| NGC 4486 | HST/STIS | N + S | Y | 395 ± 4 | 198 ± 22 | −101 ± 378 | 655 ± 18 | − | − | − |
| Palomar ( * ) | N + S + B | Y | −478 ± 4 | 238 ± 5 | 96 ± 6 | 286 ± 9 | −285 ± 145 | 908 ± 141 | 5 | |
| NGC 4552 ( † ), ( ‡ ) | HST/STIS ( ‡ ) | N + S + B | Y | −103 ± 47 | 157 ± 18 | 501 ± 38 | 249 ± 50 | 541 ± 53 | 1360 ± 20 | 70 |
| Palomar ( † ) | N | Y | 56 ± 59 | 282 ± 68 | − | − | − | − | − | |
| NGC 4594 | HST/STIS | N + S + B | N | 70 ± 15 | 108 ± 26 | 66 ± 152 | 554 ± 6 | 519 ± 120 | 1677 ± 18 | 16 |
| Palomar | N + B | Y | –11 ± 4 | 215 ± 7 | − | − | 698 ± 26 | 956 ± 41 | 33 | |
| NGC 4676B ( * ), ( ‡ ) | HST/STIS ( ‡ ) | N + B | N | 527 ± 40 | 198 ± 12 | − | − | 336 ± 16 | 748 ± 12 | 89 |
| NGC 4698 | HST/STIS | N + B | N | 55 ± 19 | 90 ± 5 | − | − | 273 ± 97 | 1375 ± 9 | 39 |
| Palomar | N | Y | −7 ± 2 | 98 ± 8 | − | − | − | − | − | |
| NGC 4736 | HST/STIS | N + B | Y | 127 ± 14 | 84 ± 12 | − | − | 330 ± 1 | 738 ± 4 | 82 |
| Palomar | N | Y | 23 ± 4 | 105 ± 10 | − | − | − | − | − |
Notes. From left to right: ID: object designation; Inst.: HST/STIS or Palomar spectra; Comp.: components used for the best-fitting model with N, S and B referring to narrow, second, and broad components, respectively; [O I]: if these lines are present in the spectrum or not (Yes/No); velocity (V) and velocity dispersion (σ) for each component for each of the reference emission lines; fblend: contribution of the broad component to the total flux of the Hα − [N II] complex. The galaxies in bold show a secondary component in the HST/STIS spectrum classified as outflow (see Sect. 6.2 and Fig. 2).
( * )Indicates that the broad component detection in Hα − [N II] lines is not well-constrained (Sect. 6.3).
( † )The data for which the O-model was used to model the emission lines (see Sect. 3.2).
( ‡ )Marks the spectra with low S/N (Sect. 2).
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