All Figures

$\begin{figure} \par\includegraphics[width=7cm,clip]{3370fig1.eps} \end{figure}$ Figure 1: DSS field image of PKS 2005-489 ( top) and PKS 2155-304 ( bottom) (B band, field of view of $10.5' \times 10.5'$ ). The stars used as reference and control in the optical and infrared observations are indicated, along with the galaxy used to study the influence of host contribution in the PKS 2005-489 light curve (see text).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{3370fig2.eps} \end{figure}$ Figure 2: Light curves of the BL Lac PKS 2005-489 in six bands during the two consecutive nights in July 2001 in which short-term variability was detected. The control light curves for the V and H bands are also shown to exemplify their stability.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3370fig3.eps} \end{figure}$ Figure 3: Light curve of the galaxy indicated in Fig. 1 (G) and the respective control light curves for the night of 07/17/01 in the R band. The absence of variations confirms that the variability detected in PKS 2005-489 light curve was not caused by the influence of the host galaxy.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3370fig4.eps} \end{figure}$ Figure 4: Comparison between the FWHM evolution and PKS 2005-489 flux density during the nights of July 16 and 17 with the V and R filters.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3370fig5.eps} \end{figure}$ Figure 5: Spectral energy distribution of PKS 2005-489 from data taken between 2001 and 2003. The error bars correspond to the standard deviation in daily averages.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{3370fig6.eps} \end{figure}$ Figure 6: Correlation between spectral indices calculated between two consecutive bands and the corresponding flux densities in PKS 2005-489. The solid lines represent a linear fit to the spectral indices. The goodness of the fit (R²) is indicated in each plot. In the last panel, the open triangules and the open squares indicate the 2002 and 2003 measurements, respectively.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=11.5cm,clip]{3370fig7.eps} \end{figure}$ Figure 7: Light curves of the BL Lac PKS 2005-489 in the V and R bands during the nights of July 16 and 17, 2001, and the spectral indices calculated between these two bands on time scales of a few minutes.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{3370fig8.eps} \end{figure}$ Figure 8: Light curve of the BL Lac PKS 2155-304 during three nights in July and August 2001 in six bands. The control light curves in the V and H band are also shown to exemplify their stability.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3370fig9.eps} \end{figure}$ Figure 9: Spectral energy distribution of PKS 2155-304 between July 2001 and May 2003 in the six filters. We binned the data for better visualization; the error bars correspond to the standard deviation of the daily averages.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{3370fig10.eps} \end{figure}$ Figure 10: Correlation between spectral indices calculated between two consecutive bands and the corresponding flux densities in PKS 2155-304. The solid lines represent a linear fit to the spectral indices. The goodness of the fit (R²) is indicated in each plot. In the last panel, the open triangle and the open square indicate the 2002 and 2003 measurements, respectively.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3370fig1.eps} \end{figure}$	Figure 1: DSS field image of PKS 2005-489 ( top) and PKS 2155-304 ( bottom) (B band, field of view of $10.5' \times 10.5'$ ). The stars used as reference and control in the optical and infrared observations are indicated, along with the galaxy used to study the influence of host contribution in the PKS 2005-489 light curve (see text).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9cm,clip]{3370fig2.eps} \end{figure}$	Figure 2: Light curves of the BL Lac PKS 2005-489 in six bands during the two consecutive nights in July 2001 in which short-term variability was detected. The control light curves for the V and H bands are also shown to exemplify their stability.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{3370fig3.eps} \end{figure}$	Figure 3: Light curve of the galaxy indicated in Fig. 1 (G) and the respective control light curves for the night of 07/17/01 in the R band. The absence of variations confirms that the variability detected in PKS 2005-489 light curve was not caused by the influence of the host galaxy.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3370fig4.eps} \end{figure}$	Figure 4: Comparison between the FWHM evolution and PKS 2005-489 flux density during the nights of July 16 and 17 with the V and R filters.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{3370fig5.eps} \end{figure}$	Figure 5: Spectral energy distribution of PKS 2005-489 from data taken between 2001 and 2003. The error bars correspond to the standard deviation in daily averages.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=5cm,clip]{3370fig6.eps} \end{figure}$	Figure 6: Correlation between spectral indices calculated between two consecutive bands and the corresponding flux densities in PKS 2005-489. The solid lines represent a linear fit to the spectral indices. The goodness of the fit (R²) is indicated in each plot. In the last panel, the open triangules and the open squares indicate the 2002 and 2003 measurements, respectively.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=11.5cm,clip]{3370fig7.eps} \end{figure}$	Figure 7: Light curves of the BL Lac PKS 2005-489 in the V and R bands during the nights of July 16 and 17, 2001, and the spectral indices calculated between these two bands on time scales of a few minutes.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=14cm,clip]{3370fig8.eps} \end{figure}$	Figure 8: Light curve of the BL Lac PKS 2155-304 during three nights in July and August 2001 in six bands. The control light curves in the V and H band are also shown to exemplify their stability.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3370fig9.eps} \end{figure}$	Figure 9: Spectral energy distribution of PKS 2155-304 between July 2001 and May 2003 in the six filters. We binned the data for better visualization; the error bars correspond to the standard deviation of the daily averages.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=5cm,clip]{3370fig10.eps} \end{figure}$	Figure 10: Correlation between spectral indices calculated between two consecutive bands and the corresponding flux densities in PKS 2155-304. The solid lines represent a linear fit to the spectral indices. The goodness of the fit (R²) is indicated in each plot. In the last panel, the open triangle and the open square indicate the 2002 and 2003 measurements, respectively.
Open with DEXTER