All Figures

$\begin{figure} \par\includegraphics[width=15cm,clip]{3943fg1.eps} \end{figure}$ Figure 1: (u,v) coverage of 0716+714 at September 29 ( left), October 4 ( middle), October 5 ( right). The individual coverage are nearly identical, which allows a reliable comparison of the obtained maps.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3943fg2.eps} \end{figure}$ Figure 2: Amplitude vs. (u,v)-distance of 0716+714 (Oct. 5). Clearly visible is the higher noise at the HALCA baselines at large (u,v)-distances. The dotted line (marginally visible in the centre of the HALCA data) represents the final clean model.
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In the text

$\begin{figure} \par\includegraphics[width=4cm,clip]{3943fg3.eps}\hspace*{2mm} \... ...g5.eps}\hspace*{2mm} \includegraphics[width=4cm,clip]{3943fg6.eps} \end{figure}$ Figure 3: An example of the tests made to check the reliability of the D-term solutions: the panels show the real ( top) and imaginary part ( bottom) of the Stokes U data on all ground array baselines to Los Alamos plotted versus the parallactic angle (Sep. 29). Left panels: before application of D-term calibration. Right panels: after the D-term calibration was applied. The calibration successfully removes the systematic variation of the amplitude with parallactic angle.
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In the text

$\begin{figure} \par\hbox{\hspace*{24mm}% \includegraphics[angle=0,width=5.9cm] {... ...75){\makebox(0,0){Oct. 5}} \put(-25,175){\makebox(0,0){Oct. 5}}} \end{figure}$ Figure 4: Left panels: ground array contour maps of Stokes I of 0716+714 with polarization vectors superimposed. The length of the polarization vectors is proportional to the intensity of the linear polarization (1 mas corresponds to 2.5 mJy/beam in P). Contours start at 0.13 mJy/beam, increasing in steps of 2. Right panels: contour maps of the linear polarization. Contours start at 0.25 mJy/beam, increasing in steps of 2. The lowest contour of the total intensity is given by the outer grey line. Time order is from top to bottom: 29 Sep., 4 Oct., and 5 Oct. 2000. The beam size, total flux density, and rms are given in the observing log, Table 1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3943fg13.ps} \end{figure}$ Figure 5: Contour images of 0716+714 at 43 GHz and 86 GHz showing that the jet is bent by about $20^\circ$ in the inner 1 mas with respect to the jet at lower resolution. Left: 43 GHz VLBA contour map at a resolution of $166 \times 196~\mu$ as at $-43.5^\circ$ from March 14, 2003. The peak flux density is 2 Jy/beam and the contours start at 6 mJy increasing in steps of 2. Middle: super resolved ( $76 \times 49~\mu$ as at $3.5^\circ$ ) version of the 43 GHz map. Right: 86 GHz map at a resolution of $76 \times 49~\mu$ as at $3.5^\circ$ from April 28, 2003. Peak flux density is 2.4 Jy/beam and the contours start at 20 mJy.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{3943fg14.ps} \end{figure}$ Figure 6: Slices along ${\rm PA}=12.5^\circ$ through the total intensity, linear polarization intensity, fractional polarization, and EVPA images of the core and the jet of 0716+714.
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In the text

$\begin{figure} \par\hbox{\hspace*{24mm} \includegraphics[bb=50 145 567 696,angl... ...75){\makebox(0,0){Oct. 5}} \put(-345,175){\makebox(0,0){Oct. 5}}} \end{figure}$ Figure 7: Left panels: VSOP contour maps of Stokes I of 0716+714 with polarization vectors superimposed (1 mas corresponds to 6.7 mJy/beam). Contours start at 1.8 mJy/beam and increasing in steps of 2. Right panels: contour maps of the linear polarization. Contours start at 1.3 mJy/beam and increasing in steps of 2. The outline of the total intensity is indicated by the outer grey contour. Time order is from top to bottom: 29 Sep., 4 Oct., and 5 Oct. 2000. The beam size, total flux density and rms are given in the observing log, Table 1. Intensity profiles through the core component that better show the variability are given in Fig. 8.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{3943fg21.ps} \end{figure}$ Figure 8: Slices along ${\rm PA}=12.5^\circ$ through the VSOP images of the core of 0716+714 in total intensity, linear polarization intensity, fractional polarization and EVPA. It is a virtual zoom into the core region of Fig. 6, and r=0 marks the same position in both plots.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3943fg22.eps} \end{figure}$ Figure 9: Total intensity ( top), linear polarization ( middle), and EVPA variations of 0716+714 and the calibrator 0836+710, as measured at Effelsberg at 5 GHz. The left panel shows the data from September 29 and the right panels from October 4 to 5 (note that the time axis between left and right panels differ). For intensity and polarization, we show relative variations, normalised to the mean (average taken over all three days). For the EVPA we plot the absolute difference relative to the mean EVPA. The mean values are given in Tables 3 and 6.
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In the text

$\begin{figure} \par\hbox{\hspace*{-0.5mm} \includegraphics[angle=-90,width=4.3cm... ...4 (03--07 UT)}} \put(-45,-16){\makebox(0,0){Oct. 4 (14--18 UT)}}} \end{figure}$ Figure 10: Linear polarization contour images of the split Oct. 4 VLBI data with polarization E-vectors superimposed. At a resolution of about 2 mas $\times$ 1 mas at $\sim$ $85^\circ$ , the contours start at 0.5 mJy/beam, increasing in steps of 2.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{3943fg1.eps} \end{figure}$	Figure 1: (u,v) coverage of 0716+714 at September 29 ( left), October 4 ( middle), October 5 ( right). The individual coverage are nearly identical, which allows a reliable comparison of the obtained maps.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3943fg2.eps} \end{figure}$	Figure 2: Amplitude vs. (u,v)-distance of 0716+714 (Oct. 5). Clearly visible is the higher noise at the HALCA baselines at large (u,v)-distances. The dotted line (marginally visible in the centre of the HALCA data) represents the final clean model.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{3943fg14.ps} \end{figure}$	Figure 6: Slices along ${\rm PA}=12.5^\circ$ through the total intensity, linear polarization intensity, fractional polarization, and EVPA images of the core and the jet of 0716+714.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{3943fg21.ps} \end{figure}$	Figure 8: Slices along ${\rm PA}=12.5^\circ$ through the VSOP images of the core of 0716+714 in total intensity, linear polarization intensity, fractional polarization and EVPA. It is a virtual zoom into the core region of Fig. 6, and r=0 marks the same position in both plots.
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$\begin{figure} \par\hbox{\hspace*{-0.5mm} \includegraphics[angle=-90,width=4.3cm... ...4 (03--07 UT)}} \put(-45,-16){\makebox(0,0){Oct. 4 (14--18 UT)}}} \end{figure}$	Figure 10: Linear polarization contour images of the split Oct. 4 VLBI data with polarization E-vectors superimposed. At a resolution of about 2 mas $\times$ 1 mas at $\sim$ $85^\circ$ , the contours start at 0.5 mJy/beam, increasing in steps of 2.
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