$\begin{figure} \par { (a)\includegraphics[width=7.25cm,clip]{0232f6a.eps}\hspace... ...ace*{2mm} (d)\includegraphics[width=7.25cm,clip]{0232f6d.eps} } \end{figure}$ Figure 6: The dependences of $\overline{\Delta\xi},~\overline{\Delta\eta}$ on magnitude before exclusion of the magnitude equation ( a), c)) and after exclusion of the magnitude equation ( b), d)).
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In the text

$\begin{figure} \par\includegraphics[width=5.6cm,clip]{0232f8.eps} \end{figure}$ Figure 8: The dependences of internal mean errors $\epsilon_{\alpha}\cos\delta$ ( $\bullet$ ) and $\epsilon _{\delta }$ ( $\times$ ) on magnitude in the Pul-3 catalogue.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{0232f1.eps} \end{figure}$	Figure 1: Distribution of the Pulkovo fields with galaxies in equatorial coordinates.
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$\begin{figure} \par\includegraphics[width=5.6cm,clip]{0232f2.eps} \end{figure}$	Figure 2: Distribution of the observing epochs. $N_{\rm pl}$ is a number of plates.
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{0232f3.eps} \end{figure}$	Figure 3: Histogram of photographic magnitudes of the Pul-3 stars.
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$\begin{figure} \par (a)\includegraphics[width=4.6cm,clip]{0232f4a.eps}\vspace*{2mm} (b)\includegraphics[width=4.6cm,clip]{0232f4b.eps} \end{figure}$	Figure 4: Dependence $\Delta \xi$ on $\tilde\xi$ for stars of 12.5 to 13.5 mag. a) before coma exclusion, b) after coma exclusion.
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$\begin{figure} \par { (a)\includegraphics[width=7.25cm,clip]{0232f5a.eps}\hspace*{2mm} (b)\includegraphics[width=7.25cm,clip]{0232f5b.eps} } \end{figure}$	Figure 5: The examples of magnitude equation $\overline {\Delta \xi }({\rm mag})$ a), $\overline {\Delta \eta }({\rm mag})$ b) for different declination zones.
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$\begin{figure} \par { (a)\includegraphics[width=7.25cm,clip]{0232f6a.eps}\hspace... ...ace*{2mm} (d)\includegraphics[width=7.25cm,clip]{0232f6d.eps} } \end{figure}$	Figure 6: The dependences of $\overline{\Delta\xi},~\overline{\Delta\eta}$ on magnitude before exclusion of the magnitude equation ( a), c)) and after exclusion of the magnitude equation ( b), d)).
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$\begin{figure} \par { \includegraphics[width=6.65cm,clip]{0232f7a.eps}\hspace*{2mm} \includegraphics[width=6.65cm,clip]{0232f7b.eps} } \end{figure}$	Figure 7: Histograms of the standard errors of positions and proper motions of stars of the Pul-3.
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$\begin{figure} \par\includegraphics[width=5.6cm,clip]{0232f8.eps} \end{figure}$	Figure 8: The dependences of internal mean errors $\epsilon_{\alpha}\cos\delta$ ( $\bullet$ ) and $\epsilon _{\delta }$ ( $\times$ ) on magnitude in the Pul-3 catalogue.
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$\begin{figure} \par {\includegraphics[width=4.3cm,clip]{0232f9a.eps}\hspace{1mm... ...\hspace{1mm} \includegraphics[width=4.3cm,clip]{0232f9d.eps} } \end{figure}$	Figure 9: The mean systematic differences (Tycho-2 - Pul-3) with dependence on declination.
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$\begin{figure} \par {\includegraphics[width=4.3cm,clip]{0232f10a.eps}\hspace{1m... ...hspace{1mm} \includegraphics[width=4.3cm,clip]{0232f10d.eps} } \end{figure}$	Figure 10: The mean systematic differences (Tycho-2 - Pul-3) with dependence on right ascension.
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