Table 2
Results of modeling the brightness distribution of the VLA observations.
| Frequency | ID | Flux density | RA | Dec |
|---|---|---|---|---|
| (GHz) | (mJy) | (″) | (″) | |
| 1.49 | A1 | 376 ± 20 | − 21.6 | 11.6 |
| A2 | 27 ± 1 | − 17.9 | 10.8 | |
| B | 674 ± 30 | 0.0 | 0.0 | |
| C1 | 168 ± 8 | 20.7 | − 18.2 | |
| C2 | 80 ± 4 | 20.4 | − 17.3 | |
| 4.86 | A1 | 239 ± 10 | − 21.6 | 11.5 |
| A2 | 6 ± 0.5 | − 17.8 | 10.8 | |
| B | 219 ± 11 | − 0.2 | − 0.2 | |
| C1 | 59 ± 5 | 20.9 | − 18.2 | |
| C2 | 19 ± 1 | 20.3 | − 17.1 | |
| 14.94 | A1 | (167 ± 2) | (−21.7) | (11.6) |
| B | 49 ± 3 | − 0.2 | − 0.2 | |
| C1 | (14 ± 3) | (20.8) | (−18.2) | |
Notes. For details on the flux density see text. In cols. 4 and 5, relative coordinates are given for the brightest component in each region. The uncertainties of the coordinates are 0.″3 at 1.49 GHz, and 0.″ 1 at 4.86 and 14.94 GHz. In the case of the 14.94 GHz observation, the parentheses indicate that at the positions of A1 and C1 bandwidth smearing is significant, which could affect the results of the modelfit.
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