Table 7.
Radii of the warm ionised gas outflows as estimated from the optical data (HST or X-shooter) (Col. 2) and the radio source radii taken from the literature (Col. 3).
| Object | roptical | rradio | Best |
|---|---|---|---|
| [kpc] | [kpc] | estimate | |
| PKS 0023–26 | 1.3 ± 0.1 | 1.53 | HST |
| PKS 0252–71 | 0.23 ± 0.02 | 0.47 | SA |
| PKS 1151–34 | ≤0.40 | 0.18 | RAD |
| PKS 1306–09 | 1.9 ± 0.2 | 1.11 | HST |
| PKS 1549–79 | 0.19 ± 0.02 | 0.35 | HST |
| PKS 1814–63 | ≤0.21 | 0.15 | RAD |
| PKS 1934–63 | 0.059 ± 0.012 ( * ) | 0.064 | SA |
| PKS 2135–209 | 0.56 ± 0.02 | 0.58 | SA |
| PKS 2314+03 | ≤0.46 | 0.36 | RAD |
Notes. The final column indicates the method used to determine the best outflow radius estimate for use when calculating general outflow properties (HST: HST narrow-band imaging; RAD: radial extent of radio source; SA: X-shooter spectro-astrometry). In most cases, Col. 3 represent half the radio source diameter values presented in the final column of Table 1, under the assumption that the radio lobes are symmetric about the nucleus. However, in the case of the core-jet source PKS 1549–79, we took the maximum extent of the radio emission on the east side of the nucleus. ( * )Radius estimated using the spectro-astrometry technique taken from Santoro et al. (2018).
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