Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{2407fig1.eps} \end{figure}$ Figure 1: The radio spectrum of J1101+7225 at different angular resolutions, corresponding to Table 3. All VLBI measurements are labelled with the observing date. While the flux densities are plotted with error bars, the stars indicate peak brightnesses. Because the peak brightnesses may underestimate the flux densities, the corresponding spectra are dotted / dashed (see Sect. 3.1).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2407fig2.eps} \end{figure}$ Figure 2: Cleaned map of the EVN observation of J1101+7225 at 1.66 GHz. The map shows a peak brightness of 407 mJy/beam. The contour levels are -0.15, 0.15, 0.3, 0.6, 1.2, 2.4, 4.8, 9.6, 19.2, 38.4, 76.8% of the peak brightness, and the beam size is $6.22\times 5.28$ mas at position angle (PA) of 4 $^\circ$ . In the upper right corner the Gaussian model fit representation of the VLBI image is given (with the same contour levels, but now with respect to a 399 mJy/beam peak brightness), obtained by fitting Gaussian components to the visibility data (beam: $5.5 \times 4.3$ mas at PA 2 $^\circ$ ). By this technique the extended structure at $\sim$ 50 mas distance to the core could be clearly resolved into two components.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2407fig3.eps} \end{figure}$ Figure 3: The cleaned maps are aligned vertically (rotation about $-20^{\circ }$ ), which is justified by the fact, that no significant change of the position angle of the jet axis was observed. The apparent linear velocities of the fitted Gaussian components (cf. Table 6) are given. The first map by T95 at T(1,1.66 GHz) shows a peak brightness of 476 mJy/beam, the contour levels are -2, -1, 1, 2, 4, 8, 16, 32, 63, 127, 253 mJy/beam, and the beam size is $4.2\times 3.2$ mas at PA 90 $^\circ$ . The second map by B02 at T(2,2.3 GHz) shows a peak brightness of 520 mJy/beam, the contour levels are -3, 3, 6, 12, 24, 48, 96, 192, 384 mJy/beam, and the beam size is $3.3\times 6.7$ mas at PA 20 $^\circ$ . The beam PAs given here refer to the unrotated coordinate system.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2407fig4.eps} \end{figure}$ Figure 4: 5 GHz maps of the central 5 mas. The details are given in the form: peak brightness; contour levels in %; beam size. First epoch: 0.097 mJy/beam; levels are -8, 8, 12, 18, 27, 40.5, 60.8%; beam: $1.08\times 0.79$ mas at PA $-70^\circ$ . Second epoch: 0.209 mJy/beam; levels are 6, 9, 13.5, 20.3, 30.4, 45.6, 68.3%; beam: $0.96\times 0.90$ mas at PA $-90^\circ$ . Third epoch: 0.314 mJy/beam; levels are 1.6, 2.56, 4.1, 6.55, 10.5, 16.8, 26.8, 42.9, 68.7, %; beam: $1.95\times 1.64$ mas at PA $-67^\circ$ . Fourth epoch: 0.417 mJy/beam; levels are -0.9, 0.9, 1.44, 2.3, 3.69, 5.9, 9.44, 15.1, 24.2, 38.7, 61.8%; beam: $2.11\times 1.64$ mas at PA $-65^\circ$ . Crosses indicate the positions of circular Gaussian modelfit components. The detailed model parameters are presented in Table 7.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2407fig5.eps} \end{figure}$ Figure 5: Evolving core-distance (in mas) of the best fit Gaussians, taken from Table 7 over the years. A least-squares fit of a linear time-dependence is shown with respect to the errorbars. The standard deviation of the resulting apparent separation velocities is $\sigma \approx 0.04$ mas yr^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{2407fig1.eps} \end{figure}$	Figure 1: The radio spectrum of J1101+7225 at different angular resolutions, corresponding to Table 3. All VLBI measurements are labelled with the observing date. While the flux densities are plotted with error bars, the stars indicate peak brightnesses. Because the peak brightnesses may underestimate the flux densities, the corresponding spectra are dotted / dashed (see Sect. 3.1).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2407fig5.eps} \end{figure}$	Figure 5: Evolving core-distance (in mas) of the best fit Gaussians, taken from Table 7 over the years. A least-squares fit of a linear time-dependence is shown with respect to the errorbars. The standard deviation of the resulting apparent separation velocities is $\sigma \approx 0.04$ mas yr^-1.
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