All Figures

$\begin{figure} \par\resizebox{3in}{!}{\includegraphics{6754fig1.eps}}\end{figure}$ Figure 1: The MERLIN archive image of 1011+496 at 1.6 GHz on May 6, 1999. The contour levels are -1, 1, 2, 4, 8, 16, 32, 64... times 0.001742 Jy beam^-1 (3 $\sigma$ ).
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{6754fig2.eps}\end{figure}$ Figure 2: Multi-epoch EVN and VLBA images at 5 GHz. The minimum contour level is 3 times the rms noise given in Table 1. The contour levels are multiples (-1, 1, 2, 4, 8, 16, 32, 64...) of the minimum contour level and the axes are labeled in milliarcseconds. The top three panels are for 1011+496 at 1997.055, 1998.493, and 1999.893 ( from left to right); the middle for 1424+240 at 1999.696, 1999.893, and 2003.447 ( from left to right); while the bottom for 1542+614 and 4C+37.46 at 1999.893.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{6754fig3.eps}\end{figure}$ Figure 3: EVN and VLBA images of 1133+704 at 5 GHz. The epoch of observation from left to right are: epoch 1997.055, epoch 1998.493, epoch 1999.893. The axes are labeled in milliarcseconds. Contours are drawn at -1, 1, 2, 4, 8, 16,... times the noise level. Numerical parameters of the images are given in Table 1.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{6754fig4.eps}}\end{figure}$ Figure 4: Positions of components with respect to the core at different epochs from model fitting for 1133+704. The data point at 1991.433 is taken from Kollgaard et al. (1996a). All the other epochs are those presented in this paper, and the lines represent the linear fitting of the motion for each jet component.
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In the text

$\begin{figure} \par\resizebox{3in}{!}{\includegraphics{6754fig5.eps}}\end{figure}$ Figure 5: The MERLIN archive image of 1424+240 at 1.6 GHz observed on 1993 Apr. 1. The contour levels are -1, 1, 2, 4, 8, 16, 32, 64... times 0.001745 Jy beam^-1(3 $\sigma$ ).
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In the text

$\begin{figure} \par\resizebox{3in}{!}{\includegraphics{6754fig6.eps}}\end{figure}$ Figure 6: The MERLIN archive image of 4C+37.46 at 5 GHz observed on 1999 May 6. The contour levels are -1, 1, 2, 4, 8, 16, 32, 64... times 0.001745 Jy beam^-1 (3 $\sigma$ ).
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{6754fig7.eps}\end{figure}$ Figure 7: EVN and VLBA images of 1727+502 at 5 GHz. The top from left to right are: epoch 1995.534, epoch 1997.055, epoch 1998.493. The bottom from left to right are: epoch 1999.893, epoch 2002.403. The axes are labeled in milliarcseconds. Contours are drawn at -1, 1, 2, 4, 8, 16,... times the noise level. Numerical parameters of the images are given in Table 1.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{6754fig8.eps}}\end{figure}$ Figure 8: Positions of components with respect to the core at different epochs from model fitting for 1727+502. The data point at 1991.433 is taken from Kollgaard et al. (1996a). All the other epochs are those presented in this paper, and the lines represent the linear fitting of the motion for each jet component.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{6754fig9.eps}\end{figure}$ Figure 9: EVN and VLBA images of 1741+196 at 5 GHz. The top from left to right are: epoch 1997.055, epoch 1997.378, epoch 1998.493. The bottom from left to right are: epoch 1999.893, epoch 2002.400, epoch 2003.447. The axes are labeled in milliarcseconds. Contours are drawn at -1, 1, 2, 4, 8, 16,... times the noise level. Numerical parameters of the images are given in Table 1.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{6754fig10.eps}}\end{figure}$ Figure 10: Positions of components with respect to the core at different epochs from model fitting for 1741+196. All the data points are presented in this paper, the lines represent the linear fitting of the motion for each jet component except the data point at 2002.400, as the baseline of this epoch is much shorter than the others.
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In the text

$\begin{figure}\resizebox{8.8cm}{!}{\includegraphics{6754fig11.eps}}\end{figure}$ Figure 11: The relationship between the radio 5 GHz extended flux and the radio low-frequency 408 MHz flux.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6754fig12.eps}\end{figure}$ Figure 12: The distribution of 408 MHz luminosity for BL Lac objects selected from Nieppola et al. (2006).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{6754fig13.eps}\end{figure}$ Figure 13: The Doppler factor versus the intrinsic synchrotron peak frequency $\nu _{\rm peak}^{'}$ (see text for details).
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In the text

$\begin{figure} \par\includegraphics[width=11.3cm,clip]{6754fig14.eps}\end{figure}$ Figure 14: The low-frequency 408 MHz luminosity versus the intrinsic synchrotron-peak frequency $\nu _{\rm peak}'$ . The open circles are the sources with the direct measurements of 408 MHz radio flux and known redshift, the open triangles are the sources calculated from either the 360 MHz, or 330 MHz radio flux with known redshift, while the solid circles are those estimated from the extended flux (at 5 GHz or 1.4 GHz), the total 1.4 GHz radio flux, or low-frequency radio flux (with unknown redshift) (see text for details).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6754fig15.eps}\end{figure}$ Figure 15: The viewing angle versus the intrinsic synchrotron peak frequency $\nu _{\rm peak}'$ . The viewing angle is estimated by assuming a Lorentz factor of 5 and using the estimated Doppler factor in Sect. 4.4. The errorbar is indicated with the viewing angle of Lorentz factors of 3 and 10.
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In the text

$\begin{figure} \par\resizebox{3in}{!}{\includegraphics{6754fig1.eps}}\end{figure}$	Figure 1: The MERLIN archive image of 1011+496 at 1.6 GHz on May 6, 1999. The contour levels are -1, 1, 2, 4, 8, 16, 32, 64... times 0.001742 Jy beam^-1 (3 $\sigma$ ).
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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{6754fig3.eps}\end{figure}$	Figure 3: EVN and VLBA images of 1133+704 at 5 GHz. The epoch of observation from left to right are: epoch 1997.055, epoch 1998.493, epoch 1999.893. The axes are labeled in milliarcseconds. Contours are drawn at -1, 1, 2, 4, 8, 16,... times the noise level. Numerical parameters of the images are given in Table 1.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{6754fig4.eps}}\end{figure}$	Figure 4: Positions of components with respect to the core at different epochs from model fitting for 1133+704. The data point at 1991.433 is taken from Kollgaard et al. (1996a). All the other epochs are those presented in this paper, and the lines represent the linear fitting of the motion for each jet component.
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$\begin{figure} \par\resizebox{3in}{!}{\includegraphics{6754fig5.eps}}\end{figure}$	Figure 5: The MERLIN archive image of 1424+240 at 1.6 GHz observed on 1993 Apr. 1. The contour levels are -1, 1, 2, 4, 8, 16, 32, 64... times 0.001745 Jy beam^-1(3 $\sigma$ ).
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$\begin{figure} \par\resizebox{3in}{!}{\includegraphics{6754fig6.eps}}\end{figure}$	Figure 6: The MERLIN archive image of 4C+37.46 at 5 GHz observed on 1999 May 6. The contour levels are -1, 1, 2, 4, 8, 16, 32, 64... times 0.001745 Jy beam^-1 (3 $\sigma$ ).
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$\begin{figure} \par\includegraphics[width=12cm,clip]{6754fig7.eps}\end{figure}$	Figure 7: EVN and VLBA images of 1727+502 at 5 GHz. The top from left to right are: epoch 1995.534, epoch 1997.055, epoch 1998.493. The bottom from left to right are: epoch 1999.893, epoch 2002.403. The axes are labeled in milliarcseconds. Contours are drawn at -1, 1, 2, 4, 8, 16,... times the noise level. Numerical parameters of the images are given in Table 1.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{6754fig8.eps}}\end{figure}$	Figure 8: Positions of components with respect to the core at different epochs from model fitting for 1727+502. The data point at 1991.433 is taken from Kollgaard et al. (1996a). All the other epochs are those presented in this paper, and the lines represent the linear fitting of the motion for each jet component.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{6754fig9.eps}\end{figure}$	Figure 9: EVN and VLBA images of 1741+196 at 5 GHz. The top from left to right are: epoch 1997.055, epoch 1997.378, epoch 1998.493. The bottom from left to right are: epoch 1999.893, epoch 2002.400, epoch 2003.447. The axes are labeled in milliarcseconds. Contours are drawn at -1, 1, 2, 4, 8, 16,... times the noise level. Numerical parameters of the images are given in Table 1.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{6754fig10.eps}}\end{figure}$	Figure 10: Positions of components with respect to the core at different epochs from model fitting for 1741+196. All the data points are presented in this paper, the lines represent the linear fitting of the motion for each jet component except the data point at 2002.400, as the baseline of this epoch is much shorter than the others.
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$\begin{figure}\resizebox{8.8cm}{!}{\includegraphics{6754fig11.eps}}\end{figure}$	Figure 11: The relationship between the radio 5 GHz extended flux and the radio low-frequency 408 MHz flux.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6754fig12.eps}\end{figure}$	Figure 12: The distribution of 408 MHz luminosity for BL Lac objects selected from Nieppola et al. (2006).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{6754fig13.eps}\end{figure}$	Figure 13: The Doppler factor versus the intrinsic synchrotron peak frequency $\nu _{\rm peak}^{'}$ (see text for details).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6754fig15.eps}\end{figure}$	Figure 15: The viewing angle versus the intrinsic synchrotron peak frequency $\nu _{\rm peak}'$ . The viewing angle is estimated by assuming a Lorentz factor of 5 and using the estimated Doppler factor in Sect. 4.4. The errorbar is indicated with the viewing angle of Lorentz factors of 3 and 10.
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