Table 5: The best fit Gaussians as mentioned in the text. a labels the major axis of elliptical Gaussians. A, B1, and B2 were only fitted by circular Gaussians, because the locations of components of lower flux density can be fitted more reliably with less degrees of freedom. The flux density errors are $\sim$ $5\%$ , the uncertainties of the location, and size of the Gaussians range between 0.2-0.5 of the beamsize depending on the respective flux density.
Flux dens. Location Size

(mJy) r (mas) $\vartheta$ (deg) a (mas) Axial ratio

Core 396 0 0 2.88 0.41@9.4 $^\circ$

C 149 3.3 14.1 1.83 0.39@ -89.4 $^\circ$

A 54 23.3 21.0 3.62 1

B1 16 47.4 17.7 6.22 1

B2 7 62.8 18.5 4.21 1

**Table 5:** The best fit Gaussians as mentioned in the text. a labels the major axis of elliptical Gaussians. A, B1, and B2 were only fitted by circular Gaussians, because the locations of components of lower flux density can be fitted more reliably with less degrees of freedom. The flux density errors are $\sim$ $5\%$ , the uncertainties of the location, and size of the Gaussians range between 0.2-0.5 of the beamsize depending on the respective flux density.
	Flux dens.	Location	Size
	(mJy)	r (mas)	$\vartheta$ (deg)	a (mas)	Axial ratio
Core	396	0	0	2.88	0.41@9.4 $^\circ$
C	149	3.3	14.1	1.83	0.39@ -89.4 $^\circ$
A	54	23.3	21.0	3.62	1
B1	16	47.4	17.7	6.22	1
B2	7	62.8	18.5	4.21	1

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations
	3 Radio properties of the quasar J1101+7225
	4 Discussion of the results
	References