All Figures

$\begin{figure} \par\includegraphics[width=11.8cm,clip]{5744f1.eps} \end{figure}$ Figure 1: $\it UBVRI$ light curves of AO 0235+164 during the observing season 2004-2005; vertical lines indicate the XMM-Newton pointings of August 2, 2004 and January 28, 2005. The ELISA contribution has been subtracted as explained in Raiteri et al. (2005).
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{5744f2.eps} \end{figure}$ Figure 2: $\it JHK$ light curves of AO 0235+164 during the observing season 2004-2005 compared to the R-band one ( top). Vertical lines are drawn to guide the eye through variations in different bands.
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In the text

$\begin{figure} \par\includegraphics[width=14.1cm,clip]{5744f3.eps} \end{figure}$ Figure 3: R-band magnitudes ( top) and radio fluxes (Jy) at different frequencies during the 2003-2005 WEBT campaign. Vertical lines mark the times of the three XMM-Newton pointings. Cubic splines on the radio data at 37, 22, 14.5, 8, and 5 GHz are plotted to better see the long-term trend. Horizontal lines indicate the mean fluxes at these frequencies. Two different symbols are used for the 37 GHz data from Metsähovi since they come from different datasets.
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In the text

$\begin{figure} \par\includegraphics[width=11.5cm,clip]{5744f4.eps} \end{figure}$ Figure 4: B-R colour indices ( bottom) compared to the R-band light curve ( top); in the top panel blue (larger) dots indicate the R data used to derive the colour indices. Horizontal lines are drawn through average values; vertical lines indicate the times of the X-ray satellite pointings, discussed in Sect. 5.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{5744f5.eps} \end{figure}$ Figure 5: Radio light curves of the source and calibrators at 10.5 GHz ( top, blue symbols) and 4.9 GHz ( bottom, red symbols) obtained with the 100 m radio telescope at Effelsberg on August 2, 2004. The two calibrators are 3C 067 (triangles) and 4C +09.11 (crosses). The horizontal lines indicate deviations of 1% from the mean flux densities, while the yellow areas highlight the period of the X-ray observations.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{5744f6.eps} \end{figure}$ Figure 6: Radio light curves of the source and calibrators at 10.5 GHz ( top, blue symbols) and 4.9 GHz ( bottom, red symbols) obtained with the 100 m radio telescope at Effelsberg on January 28, 2005. The two calibrators are 3C 067 (triangles) and 4C +09.11 (crosses). The horizontal lines indicate deviations of 1% from the mean flux densities, while the yellow areas highlight the period of the X-ray observations.
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In the text

$\begin{figure} \par\includegraphics[width=15.75cm,clip]{5744f7.eps} \end{figure}$ Figure 7: Historical optical (mag) and radio (37, 22, 14.5, 8, and 5 GHz, flux density in Jy) light curves of AO 0235+164 shifted by the indicated amount; to increase the sampling in the optical, we show R-band data after $\rm JD=2~447~000$ and R-converted B-band data before. Yellow strips highlight the periods (a, b, c, d, e, f) where a major radio (and optical) outburst is expected on the basis of a 5.6 $\pm$ 0.5 yr quasi-periodicity; periods $\alpha$ , $\beta$ , and $\gamma$ belong to an $\sim$ 8 yr characteristic time scale of variability.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{5744f8.eps} \end{figure}$ Figure 8: Power spectrum of the discrete Fourier transform ( top) and autocorrelation function ( bottom) obtained from the historical R-band light curve. In the top panel the blue dotted line indicates the level above which the significance is better than 0.001.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{5744f9.eps} \end{figure}$ Figure 9: Power spectrum of the discrete Fourier transform ( top) and autocorrelation function ( bottom) obtained from the historical 8 GHz light curve. In the top panel the blue dotted line indicates the level above which the significance is better than 0.001.
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In the text

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{5744f10.eps} \end{figure}$ Figure 10: Spectral energy distributions of AO 0235+164 during X-ray satellite pointings. The green solid line represents a cubic spline interpolation through the August 2004 data.
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In the text

$\begin{figure} \par\includegraphics[width=11.8cm,clip]{5744f1.eps} \end{figure}$	Figure 1: $\it UBVRI$ light curves of AO 0235+164 during the observing season 2004-2005; vertical lines indicate the XMM-Newton pointings of August 2, 2004 and January 28, 2005. The ELISA contribution has been subtracted as explained in Raiteri et al. (2005).
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$\begin{figure} \par\includegraphics[width=7.65cm,clip]{5744f2.eps} \end{figure}$	Figure 2: $\it JHK$ light curves of AO 0235+164 during the observing season 2004-2005 compared to the R-band one ( top). Vertical lines are drawn to guide the eye through variations in different bands.
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$\begin{figure} \par\includegraphics[width=11.5cm,clip]{5744f4.eps} \end{figure}$	Figure 4: B-R colour indices ( bottom) compared to the R-band light curve ( top); in the top panel blue (larger) dots indicate the R data used to derive the colour indices. Horizontal lines are drawn through average values; vertical lines indicate the times of the X-ray satellite pointings, discussed in Sect. 5.
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$\begin{figure} \par\includegraphics[width=7.65cm,clip]{5744f8.eps} \end{figure}$	Figure 8: Power spectrum of the discrete Fourier transform ( top) and autocorrelation function ( bottom) obtained from the historical R-band light curve. In the top panel the blue dotted line indicates the level above which the significance is better than 0.001.
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$\begin{figure} \par\includegraphics[width=7.65cm,clip]{5744f9.eps} \end{figure}$	Figure 9: Power spectrum of the discrete Fourier transform ( top) and autocorrelation function ( bottom) obtained from the historical 8 GHz light curve. In the top panel the blue dotted line indicates the level above which the significance is better than 0.001.
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$\begin{figure} \par\includegraphics[width=16.8cm,clip]{5744f10.eps} \end{figure}$	Figure 10: Spectral energy distributions of AO 0235+164 during X-ray satellite pointings. The green solid line represents a cubic spline interpolation through the August 2004 data.
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