All Figures

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{4144fig1CMJN.eps} \end{figure}$ Figure 1: The effect of anisotropic errors on the best fit parameters of the fundamental plane (Eq. (1)). The horizontal axis gives the anisotropy parameter $\alpha$ . A small value of $\alpha$ denotes that the uncertainties in the mass estimate dominate, while for large values the uncertainties of the luminosity are dominant. $\alpha = 0.5$ corresponds to isotropic errors as used by MHDM. Also shown are the best fit values of MHDM and their uncertainties. Depending on the choice of the uncertainties one can obtain values of the parameters $\xi _{\rm R}$ between 1.4 and 3 and $\xi _{\rm M}$ between -0.8 and -3.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4144fig2.eps} \end{figure}$ Figure 2: Sketch of the SED of a relativistic jet as for example observed in BL Lac objects. At lower photon energies synchrotron emission is dominant while the high energy spectrum is usually explained by inverse Compton processes. See text for details.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4144fig3CMJN.eps} \end{figure}$ Figure 3: Histogram of the scatter in the full KFC sample. The scatter can be well approximated by a Gaussian with the standard-deviation $\sigma = 0.50$ .
Open with DEXTER

In the text

$\begin{figure} \par\mbox{\includegraphics[width=6cm,clip]{4144fig4aCMJN.eps} \in... ...g4eCMJN.eps} \includegraphics[width=6cm,clip]{4144fig4fCMJN.eps} }\end{figure}$ Figure 4: On the left side we show the $\chi ^2$ map with one (solid line), two (dashed) and three sigma (dotted) levels together with the predictions of the "jet only'' model and the ADAF/jet model. The right side shows the best fit and the AGN and XRB sample. The three rows show the different samples, from Top to bottom: KFC sample, Only XRBS and LLAGN of the KFC sample, and the edited MHDM sample.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4144fig5CMJN.eps} \end{figure}$ Figure 5: Best fit for the full KFC sample if one fixes $\xi _{\rm R}$ to 1.4, which is the value found for XRBs. Only the mass scaling parameter is fitted. One finds: $\xi _{\rm M} = -0.86\pm 0.02$ and $b_{\rm X} = - 4.9$ . The intrinsic scatter increases by less than 0.01 compared to the fit in both parameters $(\sigma _{\rm int} = 0.38)$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4144fig2.eps} \end{figure}$	Figure 2: Sketch of the SED of a relativistic jet as for example observed in BL Lac objects. At lower photon energies synchrotron emission is dominant while the high energy spectrum is usually explained by inverse Compton processes. See text for details.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{4144fig3CMJN.eps} \end{figure}$	Figure 3: Histogram of the scatter in the full KFC sample. The scatter can be well approximated by a Gaussian with the standard-deviation $\sigma = 0.50$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4144fig5CMJN.eps} \end{figure}$	Figure 5: Best fit for the full KFC sample if one fixes $\xi _{\rm R}$ to 1.4, which is the value found for XRBs. Only the mass scaling parameter is fitted. One finds: $\xi _{\rm M} = -0.86\pm 0.02$ and $b_{\rm X} = - 4.9$ . The intrinsic scatter increases by less than 0.01 compared to the fit in both parameters $(\sigma _{\rm int} = 0.38)$ .
Open with DEXTER