All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{h4334F1.ps} \end{figure}$ Figure 1: BeppoSAX spectrum ( upper panel) and residuals in units of standard deviations ( lower panel), when the a photoelectrically absorbed power-law model is applied.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{h4334F2.ps} \end{figure}$ Figure 2: GIS2 ( filled dots) and GIS3 ( open circles) residuals against a power-law plus optically thin thermal plasma continuum in the 4-10 keV bands.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{h4334F3.ps} \end{figure}$ Figure 3: PDS count rates in the 13-200 keV energy band against the column density of a Compton-thick absorber covering the NGC 6251 nucleus, for different values of the scattering fraction f. The shaded area indicates the PDS detection yielded by the BeppoSAX observation of NGC 6251. f is defined by the ratio between the normalizations of the transmitted and the warm scattered components, assuming an optically thin scatterer.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{h4334F4.ps} \end{figure}$ Figure 4: Radio (6 cm), X-ray (0.5-4.5 keV) and IR (25 $\mu$ ) color-color diagram. The dotted line represents the blazar track according to the blazar unified scheme of Fossati et al. (1998). The filled circles represent the data points corresponding to the NGC 6251 ASCA and BeppoSAX observations. The cross corresponds to the Seyfert 2 sample of Mass-Hesse et al. (1995). The empty square represents the SED of radio-quiet quasars (Elvis et al. 1994).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{h4334F5.ps} \end{figure}$ Figure 5: NGC 6251 SED. Data are from not-simultaneous observations compiled by Ho (1999), save the and X-ray data (BeppoSAX, dots; this paper), and the putative EGRET detection. The dashed line represents the best radio- $\gamma$ fit SSC model; the dotted line represents the fit with an SSC model, forced to reproduce the BeppoSAX spectral shape. The ASCA spectrum ( empty circles) is shown as well for reference.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{h4334F6.ps} \end{figure}$ Figure 6: Radio between the 1 keV and the V-band flux density in: a) NGC 6251 ( filled circle); b) the blazar radio luminosity classes in the unified scenario after Fossati et al. (1998); c) ADAF models applied to a sample of nearby elliptical galaxies (Di Matteo et al. 2000; details in text). In the last case, the error bars on the y-axis represent the rms of the sample values in the corresponding radio luminosity interval.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{h4334F1.ps} \end{figure}$	Figure 1: BeppoSAX spectrum ( upper panel) and residuals in units of standard deviations ( lower panel), when the a photoelectrically absorbed power-law model is applied.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{h4334F2.ps} \end{figure}$	Figure 2: GIS2 ( filled dots) and GIS3 ( open circles) residuals against a power-law plus optically thin thermal plasma continuum in the 4-10 keV bands.
Open with DEXTER