Table 4.
Best-fit parameters and associated uncertainty for the EPG of the galaxies studied in this work.
| Galaxy | Beam | Independent | MH I, EPG | fEPG | Rg | γ | h | dvϕ/dz | vR | vz | σ |
|---|---|---|---|---|---|---|---|---|---|---|---|
| (arcsec) | voxels | (108 M⊙) | (kpc) | (kpc) | (km s−1 kpc−1) | (km s−1) | (km s−1) | (km s−1) | |||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) |
| NGC 0672 (a) | 42 × 32 | 936 | 4.9 | 0.14 | 6.3 ± 0.4 | 0.1 ± 0.1 | 1.5 ± 0.1 | −8.4 ± 0.5 | −25.8 ± 1.4 | −35.4 ± 2.4 | 25.3 ± 0.9 |
| NGC 0925 (a) | 38 × 33 | 870 | 7.6 | 0.14 | 0.9 ± 0.1 | 13.3 ± 2.1 | 2.0 ± 0.1 | −9.7 ± 0.7 | 3.3 ± 3.5 | −17.8 ± 5.6 | 21.6 ± 1.3 |
| NGC 0949 | 39 × 35 | 190 | 1.6 | 0.27 | 3.9 ± 0.8 | 0.5 ± 0.5 | 1.6 ± 0.1 | −18.0 ± 1.4 | −29.6 ± 3.5 | −19.1 ± 3.5 | 27.7 ± 1.6 |
| NGC 2403 | 30 × 29 | 4797 | 5.9 | 0.22 | 2.3 ± 0.1 | 2.6 ± 0.3 | 0.9 ± 0.1 | −11.7 ± 0.5 | −21 ± 0.9 | −9.4 ± 1.2 | 15.2 ± 0.4 |
| NGC 2541 | 34 × 34 | 634 | 7.4 | 0.15 | – | 4.9 ± 1.0 | 2.8 ± 0.1 | −6.5 ± 0.3 | −24.3 ± 1.9 | −15.9 ± 2.3 | 27.4 ± 1.0 |
| NGC 3198 | 35 × 33 | 637 | 9.8 | 0.09 | 2.1 ± 0.5 | 9.8 ± 2.8 | 1.4 ± 0.2 | −9.2 ± 1.4 | −1.5 ± 2.6 | 8.1 ± 8.9 | 23.0 ± 1.2 |
| NGC 4062 | 39 × 34 | 148 | 2.1 | 0.11 | – | 5.0 ± 2.2 | 2.5 ± 0.1 | −9.4 ± 1.0 | −25.8 ± 5.8 | −23 ± 7.5 | 34.6 ± 2.0 |
| NGC 4258 | 33 × 33 | 1422 | 6.6 | 0.11 | 6.6 ± 1.1 | 2.3 ± 0.4 | 1.4 ± 0.1 | −10.0 ± 0.5 | −17.3 ± 1.3 | −27.2 ± 3.8 | 24.8 ± 0.7 |
| NGC 4414 (b) | 39 × 33 | 194 | 5.1 | 0.12 | – | −3.7 ± 1.9 | 0.5 ± 0.3 | −58 |
−39.5 ± 4.8 | −13.1 ± 14.2 | 26.3 ± 2.9 |
| NGC 4559 | 41 × 32 | 926 | 6.0 | 0.13 | 1.9 ± 0.3 | 4.0 ± 0.9 | 1.7 ± 0.1 | −8.2 ± 0.6 | −19.8 ± 2.5 | −33.9 ± 4.1 | 21.3 ± 1.2 |
| NGC 5055 (b) | 36 × 33 | 491 | 2.6 | 0.04 | 1.1 ± 0.2 | 8.3 ± 1.5 | 0.6 ± 0.1 | −40 |
−13.7 ± 3.9 | −39.5 ± 8.6 | 20.2 ± 2.4 |
| NGC 5585 | 34 × 33 | 368 | 3.0 | 0.12 | 2.5 |
2.6 ± 1.8 | 1.4 ± 0.3 | −2.3 ± 0.8 | 0.4 ± 2.4 | 5.4 ± 4.0 | 18.5 ± 1.0 |
Notes.
(1) NGC name; (2) FWHM of the synthesised beam; (3) number of independent EPG voxels modelled, computed as the number of voxels in the masked dataset with intensity above twice the rms-noise divided by the number of voxels per resolution element (Eq. (6)); (4) H I mass of the EPG component, with an uncertainty of ∼20%; (5) ratio between MEPG and the total H I mass; (6−7) surface density parameters (Eq. (1)), a “–” indicates that the parameter is unconstrained; (8) scale height (Eq. (2)); (9) vertical rotational gradient; (10) velocity in the direction perpendicular to the rotational axis (positive values mean outflow); (11) velocity in the direction perpendicular to the disc (positive values mean outflow); (12) velocity dispersion.
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