All Figures

$\begin{figure} \par\includegraphics[bb=0 0 2411 1890,angle=0,width=17cm,clip] {0388figA.eps} \end{figure}$ Figure 1: All contour maps of 0716+714 at 5 GHz ( top row), 8 GHz ( middle) and 15 GHz ( bottom). The maps are convolved with circular beams of 1.2 mas at 5 GHz, 0.8 mas at 8 GHz and 0.5 mas at 15 GHz. Total flux density, original beam size and the level of the lowest contour at three $\sigma$ are given in the observing log (Table 1). Contours are increasing by steps of two.
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In the text

$\begin{figure} \par\includegraphics[bb=0 0 1929 1890,angle=0,width=17cm,clip] {0388figB.eps} \end{figure}$ Figure 2: All contour maps of 0716+714 at 22 GHz. The maps are convolved with a circular beam of 0.3 mas. Total flux density, original beam size and the level of the lowest contour at three $\sigma$ are given in the observing log (Table 1). Contours are increasing by steps of two.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip] {0388fig2.ps}\end{figure}$ Figure 3: Core separation as a function of time for the individual modelfit components. Data from all frequencies are combined. Possible frequency-dependent position shifts are less than 0.1 mas and are not corrected. The solid lines show the linear fits to the path for each component. To show more clearly the well-defined components we do not show two of the farthest data points of C1 at r=11.2 mas and r=11.9 mas and one data point of C2 at r=6.9 mas.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=7.8cm,clip] {0388fig3.eps}\end{figure}$ Figure 4: Core separation as a function of time for the components C5, C7, C8 and C9 separated for the different frequencies. The solid lines show the linear fits to the path for each component. Shifts between the paths at different frequencies are visible, but are typically smaller than the measured uncertainties.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=8cm,clip] {0388fig4.eps} \end{figure}$ Figure 5: The Doppler factor versus the apparent speed for constant intrinsic Lorentz factor, $\gamma$ , (solid lines) and constant viewing angles $\theta$ (dotted lines). The range of measured speeds is indicated by the dashed lines and the grey shaded area marks the possible values for $\gamma$ and $\theta$ (see text for details).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip] {0388fig5.eps} \end{figure}$ Figure 6: Flux density of the VLBI components at 22 GHz plotted versus core separation. The components fade as they travel down the jet.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip] {0388fig6.eps}\end{figure}$ Figure 7: Spectral evolution of component C7.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0388fig7.ps} \end{figure}$ Figure 8: The long term flux density variability of 0716+714 as measured at Effelsberg and with the Michigan radio telescope at 5 GHz ( top) and 15 GHz ( middle) and the spectral index ( bottom), $\alpha_{5/15~{\rm GHz}}$ . The shaded areas mark the ejection dates of the VLBI components and their uncertainties.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=8.8cm,clip] {0388fig8.eps} \end{figure}$ Figure 9: Top: position angle of the central 1 mas of the VLBI jet grouped in one year time bins. The dashed line is a sinusoidal fit to the data. The position angle of the inner jet (ejection angle) varies with a period of $\sim$ 7.4 years. Bottom: one year bins of the 22 GHz core flux density. The dashed line represents a sinusoidal fit with a fixed period of 7.4 years.
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In the text

$\begin{figure} \par\includegraphics[bb=0 0 2411 1890,angle=0,width=17cm,clip] {0388figA.eps} \end{figure}$	Figure 1: All contour maps of 0716+714 at 5 GHz ( top row), 8 GHz ( middle) and 15 GHz ( bottom). The maps are convolved with circular beams of 1.2 mas at 5 GHz, 0.8 mas at 8 GHz and 0.5 mas at 15 GHz. Total flux density, original beam size and the level of the lowest contour at three $\sigma$ are given in the observing log (Table 1). Contours are increasing by steps of two.
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$\begin{figure} \par\includegraphics[bb=0 0 1929 1890,angle=0,width=17cm,clip] {0388figB.eps} \end{figure}$	Figure 2: All contour maps of 0716+714 at 22 GHz. The maps are convolved with a circular beam of 0.3 mas. Total flux density, original beam size and the level of the lowest contour at three $\sigma$ are given in the observing log (Table 1). Contours are increasing by steps of two.
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$\begin{figure} \par\includegraphics[angle=0,width=7.8cm,clip] {0388fig3.eps}\end{figure}$	Figure 4: Core separation as a function of time for the components C5, C7, C8 and C9 separated for the different frequencies. The solid lines show the linear fits to the path for each component. Shifts between the paths at different frequencies are visible, but are typically smaller than the measured uncertainties.
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$\begin{figure} \par\includegraphics[angle=0,width=8cm,clip] {0388fig4.eps} \end{figure}$	Figure 5: The Doppler factor versus the apparent speed for constant intrinsic Lorentz factor, $\gamma$ , (solid lines) and constant viewing angles $\theta$ (dotted lines). The range of measured speeds is indicated by the dashed lines and the grey shaded area marks the possible values for $\gamma$ and $\theta$ (see text for details).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip] {0388fig5.eps} \end{figure}$	Figure 6: Flux density of the VLBI components at 22 GHz plotted versus core separation. The components fade as they travel down the jet.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip] {0388fig6.eps}\end{figure}$	Figure 7: Spectral evolution of component C7.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0388fig7.ps} \end{figure}$	Figure 8: The long term flux density variability of 0716+714 as measured at Effelsberg and with the Michigan radio telescope at 5 GHz ( top) and 15 GHz ( middle) and the spectral index ( bottom), $\alpha_{5/15~{\rm GHz}}$ . The shaded areas mark the ejection dates of the VLBI components and their uncertainties.
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$\begin{figure} \par\includegraphics[angle=0,width=8.8cm,clip] {0388fig8.eps} \end{figure}$	Figure 9: Top: position angle of the central 1 mas of the VLBI jet grouped in one year time bins. The dashed line is a sinusoidal fit to the data. The position angle of the inner jet (ejection angle) varies with a period of $\sim$ 7.4 years. Bottom: one year bins of the 22 GHz core flux density. The dashed line represents a sinusoidal fit with a fixed period of 7.4 years.
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