Table 5.
General properties of the radio structures.
| Source |
 |
Related to AGN? | Nature of | JGI? | Ref. |
|---|---|---|---|---|---|
| [kpc] | radio features | ||||
| (1) | (2) | (3) | (4) | (5) | (6) |
| J0802+25 | < 2 | Yes | Unknown | Yes | V14 |
| J0841+01 | 40 | Yes | Core, jet or lobe or hot spot | Yes | |
| J0853+38 | 472 | Yes | Core, inner collimated jets (∼4.5 and 9 kpc), large-scale jet (∼60 kpc) | Yes | |
| radio hot spot, large and distant radio lobes (∼472 kpc) | |||||
| J0907+46 | 76 | Yes | Core, inner collimated jets | Yes | |
| large-scale bent jet (∼56 kpc) | |||||
| J0945+17 | 11 | Yes | Small (∼2.3 kpc) jet, large-scale (∼11 kpc) jet or lobe | Yes | J19 |
| J0948+25 | ∼4 | Unknown | Unknown | No | |
| J1000+12 | 43 | Yes | Core, jet-like structure (∼2.6 kpc) | Yes | J19 |
| hot spots, large-scale distorted lobes (43 kpc) | |||||
| J1108+06 | 9 | Yes (*) | Multiple components | No | B16 |
| AGN radio core, extended star formation | |||||
| J1316+44 | ≤2 | Unknown | Consistent with SF | No | |
| J1356+10 | 160 | Yes | Jet (∼5 kpc) | Yes | J19 |
| large-scale (160 kpc) radio lobes | |||||
| J1437+30 | ∼2.5 | Yes | Unknown | Yes? | |
| J1517+33 | 9 | Yes | Core, bipolar bent jet (∼9 kpc) | Yes | R10 |
| Teacup | 19 | Yes | Small-scale (∼1 kpc) radio jet | Yes | H15,R17,J19 |
| radio bubbles (∼12 kpc) (lobes/AGN wind?) |
Notes. (2) 
: radio source size in kpc. Upper limits are provided for spatially unresolved or marginally resolved (J1316+44) sources; (3) consideration of whether there are radio structures related to the nuclear activity, at least partially; (4) morphological classification of prominent radio features; (5) considering whether there is evidence for jet-gas interactions; (6) The Teacup is shown separately because it was not part of our VLA sample. The radio information comes from H15 and J19. (*)According to Bondi et al. (2016) the extended radio emission in J1108+06 is due to star formation and the radio core is associated with one of the two AGN.
References. R10: Rosario et al. (2010); V14: Villar-Martín et al. (2014); H15: Harrison et al. (2015); B16: Bondi et al. (2016); R17: Ramos Almeida et al. (2017); J19: Jarvis et al. (2019).
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