All Figures

$\begin{figure} \par\scalebox{0.6}[0.6]{\rotatebox{0}{\includegraphics{7155f1_1.e... ...0.6]{\rotatebox{0}{\includegraphics{7155f1_3.eps}}}\hspace*{6.3cm}\end{figure}$ Figure 1: The naturally-weighted VLBA maps of 3C 66A at 2.3, 8.4, and 22.2 GHz from top to bottom. The circles superimposed on the maps represent the Gaussian model components listed in Table 2, whose names are labelled. The crosses represent the restoring beams in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{7155f2_1.eps}\hspace*{4mm}... ...eps}\hspace*{4mm} \includegraphics[width=8.4cm,clip]{7155f2_4.eps} \end{figure}$ Figure 2: The spectra of VLBI components in 3C 66A: a) and b) are the spectrum of core (k component) at 2001.20 and 2001.48, and c) is the spectra of the jet components b, d, e, f, and g at 2001.20. Shown in d) is an SSA fitting curve to the spectrum of k component with all the data points from our observations at 2001.48 except 5 GHz data from Taylor et al. (1996).
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In the text

$\begin{figure} \par\mbox{ \includegraphics[width=85mm]{7155f3_1.eps} \includegraphics[width=85mm]{7155f3_2.eps} }\end{figure}$ Figure 3: The linear fitting to the separations of components b, d, e, f, and g at 2.3 and 8.4 GHz, respectively. Fitting results are given in Table 4.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{7155f4.eps} \end{figure}$ Figure 4: Identification of our jet components with the jet components detected in J01, J05, and B05. The open symbols represent our components (a, b, c, and d), filled symbols represent the components (J05-C4, J05-C3, J05-C2, J05-C1, J05-B4, J05-B6, J05-A1, and J05-A2) in J05, the half-filled symbols represent the components (J01-B1, J01-B4, and J01-B6) in J01, and the line-composed symbols represent the components (B05-B2, B05-B3, B05-C1, B05-C2, and B05-C3) in B05. See text for more details.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{7155f5.eps} \end{figure}$ Figure 5: The distribution of the flux density of the jet components against the separation from the core at 43 GHz. The data are from J05. This figure shows that the flux density of the jet component starts to increase from about 1.2 mas till about 2.6 mas (indicated by two vertical lines).
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In the text

$\begin{figure} \par\scalebox{0.6}[0.6]{\rotatebox{0}{\includegraphics{7155f1_1.e... ...0.6]{\rotatebox{0}{\includegraphics{7155f1_3.eps}}}\hspace*{6.3cm}\end{figure}$	Figure 1: The naturally-weighted VLBA maps of 3C 66A at 2.3, 8.4, and 22.2 GHz from top to bottom. The circles superimposed on the maps represent the Gaussian model components listed in Table 2, whose names are labelled. The crosses represent the restoring beams in Table 1.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{7155f2_1.eps}\hspace{4mm}... ...eps}\hspace{4mm} \includegraphics[width=8.4cm,clip]{7155f2_4.eps} \end{figure}$	Figure 2: The spectra of VLBI components in 3C 66A: a) and b) are the spectrum of core (k component) at 2001.20 and 2001.48, and c) is the spectra of the jet components b, d, e, f, and g at 2001.20. Shown in d) is an SSA fitting curve to the spectrum of k component with all the data points from our observations at 2001.48 except 5 GHz data from Taylor et al. (1996).
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$\begin{figure} \par\mbox{ \includegraphics[width=85mm]{7155f3_1.eps} \includegraphics[width=85mm]{7155f3_2.eps} }\end{figure}$	Figure 3: The linear fitting to the separations of components b, d, e, f, and g at 2.3 and 8.4 GHz, respectively. Fitting results are given in Table 4.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{7155f5.eps} \end{figure}$	Figure 5: The distribution of the flux density of the jet components against the separation from the core at 43 GHz. The data are from J05. This figure shows that the flux density of the jet component starts to increase from about 1.2 mas till about 2.6 mas (indicated by two vertical lines).
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