All Figures

$\begin{figure} \par\includegraphics[width=8.2cm,height=8.4cm,clip]{9810f1a.ps}\h... ...e*{3mm} \includegraphics[width=8.2cm,height=8.28cm,clip]{9810f1b.ps}\end{figure}$ Figure 1: Example of the procedure followed to determine the Bondi power for NGC 7898: in the left panel, we show the spectrum extracted in four annuli, centered on the nucleus, that was modeled with a PROJECT*PHA(MEKAL+POWERLAW) law; in the right panel, we show the corresponding deprojected temperature profile of the annuli.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,height=8.2cm,clip]{9810f2a.eps}\... ...ce*{3mm} \includegraphics[width=8.2cm,height=8.2cm,clip]{9810f2b.ps}\end{figure}$ Figure 2: Example of the procedure followed in this work to determine the Bondi power for NGC 7898: in the left panel, we present the X-ray surface brightness profile of the galaxy; in the right panel, we show the derived deprojected electron density profile and the power-law extrapolation used to estimate its value at the Bondi radius (marked with a diamond).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{9810f3.ps}\end{figure}$ Figure 3: Example of the procedure followed to determine the density at the Bondi radius in the case of 3C 83.1. The dotted (dashed-dotted) line represents the best-fit linear relation to the density profile obtained by using the innermost 3 (6) density measurements, while the diamond (star) is its extrapolation to the Bondi radius. The adopted value for $n_{\rm e}$ is the filled circle at $r_{\rm B}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{9810f4.ps}\end{figure}$ Figure 4: Bondi accretion power versus jet power. The stars represent FR I objects, the circles are the CoreG and the triangles represent the objects from Allen et al. sample. We also plot the best-fit linear relation (solid line).
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In the text

$\begin{figure} \par\includegraphics[width=5.4cm,clip]{9810f5a.ps}\includegraphic... ....4cm,clip]{9810f5b.ps}\includegraphics[width=5.4cm,clip]{9810f5c.ps}\end{figure}$ Figure 5: The electron density at $r_{\rm B}$ versus the jet power ( left panel) for the sub sample of 23 objects for which we are able to measure the accretion power, with the linear best-fit linear relation. Middle panel) black-hole masses versus the jet power for this same sub sample. In the right panel, we compare the linear correlation (dashed line) obtained from the 23 objects (surrounded by a large circle) with that obtained from the entire sample studied (44 objects).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{9810f6a.ps}\includegraphics[width=7.8cm,clip]{9810f6b.ps}\end{figure}$ Figure 6: Left panel: surface brightness profiles of the 23 objects, zooming into the region around a radius of 1 kpc. They are described well by power laws, with a relatively small range of slopes, while they differ substantially in normalization. Right panel: surface brightness at 1 kpc ( ${\cal S}_{1~{\rm kpc}}$ ) in units of counts s^-1 arcsec^-2, versus the jet power for the extended sample of 43 galaxies. The solid line represents the best fit linear relation.
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In the text

$\begin{figure} \par\includegraphics[width=3.6cm,clip]{9810fa01.ps}\includegraphi... ...cm,clip]{9810fa19.ps}\includegraphics[width=3.6cm,clip]{9810fa20.ps}\end{figure}$ Figure A.1: The X-ray surface brightness profiles of the 43 galaxies of the sample, having excluded UGC 7203.
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In the text

$\begin{figure}\par\includegraphics[width=3.6cm,clip]{9810fa21.ps}\includegraphic... ...m,clip]{9810fa39.ps}\includegraphics[width=3.6cm,clip]{9810fa40.ps} \end{figure}$ Figure A.1: continued.
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In the text

$\begin{figure}\par\includegraphics[width=3.6cm,clip]{9810fa41.ps}\includegraphic... ...m,clip]{9810fa42.ps}\includegraphics[width=3.6cm,clip]{9810fa43.ps} \end{figure}$ Figure A.1: continued.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{9810fa51.ps}\includegraphics... ...=5cm,clip]{9810fa64.ps}\includegraphics[width=5cm,clip]{9810fa65.ps}\end{figure}$ Figure A.2: The electron density profiles of the 30 objects, whose data quality is sufficient to perform the deprojection of the brightness profile (see Sect. 3.5). The solid lines represent the best-fit power-law relation to the density profile.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{9810fa66.ps}\includegraphics... ...5cm,clip]{9810fa79.ps}\includegraphics[width=5cm,clip]{9810fa80.ps} \end{figure}$ Figure A.2: continued.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,height=8.4cm,clip]{9810f1a.ps}\h... ...e*{3mm} \includegraphics[width=8.2cm,height=8.28cm,clip]{9810f1b.ps}\end{figure}$	Figure 1: Example of the procedure followed to determine the Bondi power for NGC 7898: in the left panel, we show the spectrum extracted in four annuli, centered on the nucleus, that was modeled with a PROJECTPHA(MEKAL+POWERLAW) law; in the right panel*, we show the corresponding deprojected temperature profile of the annuli.
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$\begin{figure} \par\includegraphics[width=8.5cm,height=8.2cm,clip]{9810f2a.eps}\... ...ce*{3mm} \includegraphics[width=8.2cm,height=8.2cm,clip]{9810f2b.ps}\end{figure}$	Figure 2: Example of the procedure followed in this work to determine the Bondi power for NGC 7898: in the left panel, we present the X-ray surface brightness profile of the galaxy; in the right panel, we show the derived deprojected electron density profile and the power-law extrapolation used to estimate its value at the Bondi radius (marked with a diamond).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{9810f4.ps}\end{figure}$	Figure 4: Bondi accretion power versus jet power. The stars represent FR I objects, the circles are the CoreG and the triangles represent the objects from Allen et al. sample. We also plot the best-fit linear relation (solid line).
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$\begin{figure} \par\includegraphics[width=3.6cm,clip]{9810fa01.ps}\includegraphi... ...cm,clip]{9810fa19.ps}\includegraphics[width=3.6cm,clip]{9810fa20.ps}\end{figure}$	Figure A.1: The X-ray surface brightness profiles of the 43 galaxies of the sample, having excluded UGC 7203.
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$\begin{figure}\par\includegraphics[width=3.6cm,clip]{9810fa21.ps}\includegraphic... ...m,clip]{9810fa39.ps}\includegraphics[width=3.6cm,clip]{9810fa40.ps} \end{figure}$	Figure A.1: continued.
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$\begin{figure} \par\includegraphics[width=5cm,clip]{9810fa51.ps}\includegraphics... ...=5cm,clip]{9810fa64.ps}\includegraphics[width=5cm,clip]{9810fa65.ps}\end{figure}$	Figure A.2: The electron density profiles of the 30 objects, whose data quality is sufficient to perform the deprojection of the brightness profile (see Sect. 3.5). The solid lines represent the best-fit power-law relation to the density profile.
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$\begin{figure} \par\includegraphics[width=5cm,clip]{9810fa66.ps}\includegraphics... ...5cm,clip]{9810fa79.ps}\includegraphics[width=5cm,clip]{9810fa80.ps} \end{figure}$	Figure A.2: continued.
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