All Figures

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{H4320F1A.ps}\includegraphics[width=8.7cm,clip]{H4320F1B.ps} \end{figure}$ Figure 1: Adaptively-smoothed Chandra ACIS-I images of 2 BL Lacs. North is up and East to the left. In PKS 0548-322, diffuse X-ray emission on cluster scales is apparent, while the image of 1ES 2344+514 exhibits a point source embedded in diffuse emission on the scale of the galaxy's halo.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4320F2.ps} \end{figure}$ Figure 2: Example of energy histogram for 1ES 2321+419, illustrating the procedure needed for the composite PSF (see text). The energies, E, and weights, W, for the monochromatic PSFs are indicated by the dashed lines.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8.6cm]{H4320F3A.ps} }\hspace*{7m... ...3E.ps} }\hspace*{7mm}{\includegraphics[width=8.6cm]{H4320F3F.ps} }\end{figure}$ Figure 3: ACIS radial profiles for each source of the sample (data points). The composite PSF, derived by merging several monochromatic PSFs (see text), is shown superimposed to the data (dashed line); the horizontal dotted line marks the background. For PKS 0548-322, PKS 2005-489, and BL Lac, excess X-ray counts over the PSF are present at radii $\protect\ga$ 20 $^{\prime \prime }$ , indicating diffuse X-ray emission around the core. Weak extended emission is also present for 1ES 2321+419 and 1ES 2344+514, while the profile for 3C 371 is entirely consistent with the instrumental PSF.
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In the text

$\begin{figure} \par\includegraphics[height=7.5cm,width=8.8cm,clip]{H4320F4A.ps}\... ...*{2mm} \includegraphics[height=7.5cm,width=8.8cm,clip]{H4320F4B.ps} \end{figure}$ Figure 4: Radial profiles and best-fit $\beta$ -model for PKS 0548-322 and PKS 2005-489. In both cases, a single $\beta$ -model was fitted to the data. However, two components for the diffuse emission are present, the first one on the scale of the host galaxy ( $\sim$ 40 $^{\prime \prime }$ ), and the second on the scale of the cluster ( $\sim$ 130-150 $^{\prime \prime }$ ). See text for further details.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4320F5A.ps}\par\vspace*{2mm} \includegraphics[width=8.8cm,clip]{H4320F5B.ps} \end{figure}$ Figure 5: X-ray contours in the energy range 0.3-8 keV overlaid on the optical images obtained from the 2.4 m Mount Palomar Telescope (POSS) archive for PKS 0548-322 (top) and PKS 2005-489 (bottom). The serendipitous X-ray sources detected with wavdetect (see text and Table 5) are marked with capital letters. North is to the top and East to the left.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{H4320F1A.ps}\includegraphics[width=8.7cm,clip]{H4320F1B.ps} \end{figure}$	Figure 1: Adaptively-smoothed Chandra ACIS-I images of 2 BL Lacs. North is up and East to the left. In PKS 0548-322, diffuse X-ray emission on cluster scales is apparent, while the image of 1ES 2344+514 exhibits a point source embedded in diffuse emission on the scale of the galaxy's halo.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4320F2.ps} \end{figure}$	Figure 2: Example of energy histogram for 1ES 2321+419, illustrating the procedure needed for the composite PSF (see text). The energies, E, and weights, W, for the monochromatic PSFs are indicated by the dashed lines.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4320F5A.ps}\par\vspace*{2mm} \includegraphics[width=8.8cm,clip]{H4320F5B.ps} \end{figure}$	Figure 5: X-ray contours in the energy range 0.3-8 keV overlaid on the optical images obtained from the 2.4 m Mount Palomar Telescope (POSS) archive for PKS 0548-322 (top) and PKS 2005-489 (bottom). The serendipitous X-ray sources detected with `wavdetect` (see text and Table 5) are marked with capital letters. North is to the top and East to the left.
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