Table 3.
Model components of the fit of circular Gaussians on the uv-plane for VLBI observations.
| Epoch | Comp. (a) | S | θ | Tb |
|---|---|---|---|---|
| (mJy) | (mas) | (105 K) | ||
| 2007.863 | 1 | 3.4 ± 0.5 | 1.41 ± 0.18 | 420 |
| 2 | 1.3 ± 0.2 | 0.60 ± 0.10 | 890 | |
| 2010.816 | 1 | 2.31 ± 0.17 | 1.30 ± 0.09 | 340 |
| 2 | 1.20 ± 0.16 | 1.51 ± 0.18 | 130 | |
| 2013.625 | 1a | 2.7 ± 0.2 | 0.90 ± 0.08 | 830 |
| 1b | 0.80 ± 0.15 | 0.40 ± 0.07 | 1200 | |
| 2 | 1.48 ± 0.19 | 0.65 ± 0.08 | 870 | |
| 2017.452 (b) | 1 | 1.2 ± 0.6 | 4.9 ± 1.3 | 1.5 |
| 2018.101 | 1 | 4.8 ± 0.8 | 11 ± 2 | 350 |
Notes.
We adopt the convention that the central component will be denoted by subindex 1. In case of detection, the subindex 2 will indicate the presence of a second component to the east. In 2013, subindices 1a and 1b indicate the central and the closest component to the east, respectively, while subindex 2 the furthest one. S represents the flux density, θ the deconvolved FWHM diameter of the circular Gaussian component and Tb the minimum brightness temperature.
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