All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3641_f1.ps} \end{figure}$ Figure 1: Spectral best fit with a broken power law of the LECS and MECS data of the 2001, July 29-30 observation of 3C 66A.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3641_f2.ps} \end{figure}$ Figure 2: The IR-optical to X-ray Spectral Energy Distribution of 3C 66A in the two BeppoSAX observations. Log-parabolic models of the synchrotron component are shown. J, H and K points (open triangles) are derived from our measurements taken one month after the BeppoSAX observation (Nesci et al. 2003) and have been reduced by 0.3 mag to match the optical fluxes as explained in Sect. 4.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3641_f3.ps} \end{figure}$ Figure 3: Spectral best fit with a single power law of the LECS and MECS data of ON 325. Note the systematic excess at energies greater than about 5 keV.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3641_f4.ps} \end{figure}$ Figure 4: Spectral best fit with a broken power law of the LECS and MECS data of ON 325.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3641_f5.ps} \end{figure}$ Figure 5: The IR to X-ray SED of ON 325. The dotted line is a log-parabolic interpolation of data.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{3641_f6.ps} \end{figure}$ Figure 6: Comparison between the Spectral Energy Distributions of the synchrotron component in some BL Lac objects measured in the observer (upper panel) and in the source frames (lower panel). The latter has been computed for an isotropic emission. All the distributions are modelled by means of log-parabolic laws: those for OJ 287 and MS 1458+22 are taken from Massaro et al. (2003a) and that for S5 1803+78, corresponding to its highest optical brightness, is taken from Massaro (2002).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3641_f7.ps} \end{figure}$ Figure 7: The SED of 3C 66A from the near IR to $\gamma$ -rays, obtained by our 2001 measurements combined with non simultaneous EGRET data according the spectrum by Lin et al. (1999) (open box) or the flux estimates above 300 MeV by Kuiper et al. (2000) (open circles). The dotted and dash-dotted lines represent possible IC components.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3641_f1.ps} \end{figure}$	Figure 1: Spectral best fit with a broken power law of the LECS and MECS data of the 2001, July 29-30 observation of 3C 66A.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3641_f2.ps} \end{figure}$	Figure 2: The IR-optical to X-ray Spectral Energy Distribution of 3C 66A in the two BeppoSAX observations. Log-parabolic models of the synchrotron component are shown. J, H and K points (open triangles) are derived from our measurements taken one month after the BeppoSAX observation (Nesci et al. 2003) and have been reduced by 0.3 mag to match the optical fluxes as explained in Sect. 4.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3641_f3.ps} \end{figure}$	Figure 3: Spectral best fit with a single power law of the LECS and MECS data of ON 325. Note the systematic excess at energies greater than about 5 keV.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3641_f4.ps} \end{figure}$	Figure 4: Spectral best fit with a broken power law of the LECS and MECS data of ON 325.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3641_f5.ps} \end{figure}$	Figure 5: The IR to X-ray SED of ON 325. The dotted line is a log-parabolic interpolation of data.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3641_f7.ps} \end{figure}$	Figure 7: The SED of 3C 66A from the near IR to $\gamma$ -rays, obtained by our 2001 measurements combined with non simultaneous EGRET data according the spectrum by Lin et al. (1999) (open box) or the flux estimates above 300 MeV by Kuiper et al. (2000) (open circles). The dotted and dash-dotted lines represent possible IC components.
Open with DEXTER