All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2391fig1.ps} \end{figure}$ Figure 1: The rms deviation of the faint reference stars as a function of instrumental magnitude for the Loiano (squares) and Asiago (crosses) data. The continuous line marks the adopted boundary between true variability and photometric uncertainty (see text).
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In the text

$\begin{figure} \par\includegraphics[width=15.7cm,clip]{2391fig2.ps} \end{figure}$ Figure 2: Light curves of 2BL candidates: abscissa is in Julian Date -2 450 000, ordinate is R mag. The triangle on the left of the vertical bar indicates the value from Londish et al. (2002) located at arbitrary JD. Black dots are our CCD data with error bars derived from the internal consistency of the faint reference stars in the data set. The dashed line is the average value of the source in the data set; the dotted lines indicate the $\pm$ $1\sigma$ strip (see text).
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In the text

$\begin{figure} \par\includegraphics[width=15.7cm,clip]{2391fig3.ps} \end{figure}$ Figure 3: Light curves of 2BL candidates: abscissa is in Julian Date -2 450 000, ordinate is R mag. Symbols as in Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[width=15.7cm,clip]{2391fig4.ps} \end{figure}$ Figure 4: Light curves of 2BL candidates: abscissa is in Julian Date -2 450 000, ordinate is R mag. Symbols as in Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[width=15.7cm,clip]{2391fig5.ps} \end{figure}$ Figure 5: Light curves of 2BL candidates: abscissa is in Julian Date -2 450 000, ordinate is R mag. Symbols as in Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[width=15.7cm,clip]{2391fig6.ps} \end{figure}$ Figure 6: Light curves of 2BL candidates: abscissa is in Julian Date -2 450 000, ordinate is R mag. Symbols as in Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[height=7.3cm,width=7.8cm,clip]{2391fig7.ps} \end{figure}$ Figure 7: The Spectral Energy Distributions (SED) of two radio-loud BL Lac objects in the 2BL sample: 1218-01 (filled circles) and 1055-01 (crosses) derived from our photometry, 2MASS and other literature data. Optical points of 1218-01 are also representative of its variability. Short dashed lines are the SEDs modelled with Eq. (1) and the long dashed line corresponds to a flat radio spectrum at a flux density of 5 mJy.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2391fig1.ps} \end{figure}$	Figure 1: The rms deviation of the faint reference stars as a function of instrumental magnitude for the Loiano (squares) and Asiago (crosses) data. The continuous line marks the adopted boundary between true variability and photometric uncertainty (see text).
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$\begin{figure} \par\includegraphics[width=15.7cm,clip]{2391fig3.ps} \end{figure}$	Figure 3: Light curves of 2BL candidates: abscissa is in Julian Date -2 450 000, ordinate is R mag. Symbols as in Fig. 2.
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$\begin{figure} \par\includegraphics[width=15.7cm,clip]{2391fig4.ps} \end{figure}$	Figure 4: Light curves of 2BL candidates: abscissa is in Julian Date -2 450 000, ordinate is R mag. Symbols as in Fig. 2.
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$\begin{figure} \par\includegraphics[width=15.7cm,clip]{2391fig5.ps} \end{figure}$	Figure 5: Light curves of 2BL candidates: abscissa is in Julian Date -2 450 000, ordinate is R mag. Symbols as in Fig. 2.
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$\begin{figure} \par\includegraphics[width=15.7cm,clip]{2391fig6.ps} \end{figure}$	Figure 6: Light curves of 2BL candidates: abscissa is in Julian Date -2 450 000, ordinate is R mag. Symbols as in Fig. 2.
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