Table 1 Model fitting parameters.

From: Evolving parsec-scale radio structure in the most distant blazar known

Epoch (yyyy mm dd)

Comp

Stotal (mJy)

Dmaj (mas)

Dmin (mas)

φ (°)

R (mas)

PA (°)

TB (×1010 K)

(1)

(2)

(3)

(4)

(5)

(6)

(7)

(8)

(9)

2004 02 27

C

119.5 ± 6.3

0.206 ± 0.005

0.041 ± 0.001

40.9 ± 0.9

47.5 ± 3.0

J1

7.2 ± 0.7

0.396 ± 0.051

0.825 ± 0.068

222.2 ± 1.1

2004 11 22

C

127.3 ± 6.6

0.269 ± 0.002

0.065 ± 0.002

28.1 ± 0.1

24.4 ± 1.5

J1

8.7 ± 0.8

0.279 ± 0.027

0.906 ± 0.064

225.0 ± 0.3

2005 03 22 & 2005 05 15

C

122.7 ± 6.4

0.209 ± 0.001

0.067 ± 0.002

55.3 ± 0.1

31.0 ± 1.8

J1

8.4 ± 0.6

0.267 ± 0.007

0.944 ± 0.052

224.7 ± 0.2

J2

1.9 ± 0.3

0.321 ± 0.053

 

1.290 ± 0.061

179.8 ± 1.3

2017 09 11

C

43.4 ± 2.3

0.260 ± 0.001

0.032 ± 0.001

49.4 ± 0.1

18.0 ± 1.1

J1

20.4 ± 1.1

0.291 ± 0.001

0.814 ± 0.049

222.2 ± 0.1

J2

1.0 ± 0.1

0.270 ± 0.033

1.568 ± 0.053

184.6 ± 0.1

2018 01 31

C

41.8 ± 2.2

0.249 ± 0.004

<0.034

52.2 ± 1.3

>17.1

J1

18.0 ± 1.0

0.170 ± 0.001

0.801 ± 0.071

222.8 ± 0.1

J2

1.4 ± 0.2

0.444 ± 0.079

1.435 ± 0.076

184.8 ± 0.9

  1. Parameters are derived from modelled Stokes LL images. Column (1) presents the observation epoch. Column (2) gives the label of the VLBI components. Column (3) presents the integrated flux density of all VLBI components. Columns (4) to (5) give the major and (in case of ellipticals) the minor axis sizes (FWHM) of the fitted Gaussian models. Column (6) is the position angle of the major axis of Gaussian, measured from north to east. The data from 22 March 2005 and 15 May were combined before model fitting. Columns (7) and (8) give the radial distance R of components with respect to the core, and the position angle measured from north to east. Column (9) lists the calculated brightness temperature of the core. For the unresolved core, a maximum size is estimated, thus the lower limit of TB is given