All Figures

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3558fig1.ps}\end{figure}$ Figure 1: Adaptively smoothed 0.3-10 keV Chandra image of Mrk 273 with a smoothing scale of 2 pixels ( $\approx$ 1''). The circle has a radius of 10'' and it is centered at the peak of the hard X-ray emission. The ellipse has a size of $42'' \times 25''$ and a position angle of $13\hbox {$^\circ $ }$ . The bright source visible in the upper left corner is Mrk 273x.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{3558fig2.ps}\end{figure}$ Figure 2: The 4.0-10 keV EPIC-PN spectrum fitted with a simple absorbed power law model ( $\Gamma$ is fixed to 1.9). Residuals are found at Fe K $\alpha$ emission line energy (at about 6.5 keV).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.38cm,clip]{3558fig3.ps}\end{figure}$ Figure 3: A simple absorbed power law model applied to the EPIC-PN spectrum of Mrk 273. Strong residuals (data/model) are clearly present above 4 keV and also between 0.6 and 1 keV.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{3558fi4a.ps}\par\includegraphics[angle=-90,width=8.3cm,clip]{3558fi4b.ps}\par\end{figure}$ Figure 4: ( Upper panel) The EPIC-PN spectrum of Mrk 273 fitted with three different temperature APEC models, a highly absorbed power law and a neutral Fe K $\alpha$ line. Each model component is displayed. ( Lower panel) The EPIC-PN and the two MOS combined fit with the same model. The closed and open circles correspond to the two MOS data sets. The best fit parameters are given in Table 2.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{3558fig5.ps}\end{figure}$ Figure 5: The EPIC-PN spectrum fitted with two thermal plasma components, a highly absorbed and a less absorbed power law with the same spectral index, plus a narrow Fe K $\alpha$ line at 6.4 keV. The best fit parameters for this model are given in Table 3.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.2cm,clip]{3558fig6.ps}\par\end{figure}$ Figure 6: The 0.3-8 keV ACIS-S spectrum of the inner 10'' region fitted with two thermal plasma components, a highly absorbed power law and a narrow Fe K $\alpha$ line at 6.4 keV. The best fit parameters are given in Table 4.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.3cm,clip]{3558fig7.ps}\par\end{figure}$ Figure 7: The 0.3-8 keV ACIS-S spectrum of the inner 10'' region fitted with a single thermal plasma component, a highly absorbed and a less absorbed power law with the same spectral index, plus a narrow Fe K $\alpha$ line at 6.4 keV. The best fit parameters are given in Table 4.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.1cm,clip]{3558fig8.ps}\end{figure}$ Figure 8: The 0.5-0.9 keV unbinned spectrum of the extended hot gas halo. A single APEC model with a temperature of $0.38\pm 0.04$ keV provides a satisfactory fit.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.1cm,clip]{3558fig9.ps}\end{figure}$ Figure A.1: The combined MOS 1 and MOS2 0.3-10 keV data fitted with a power law modified by Galactic absorption.

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3558fig1.ps}\end{figure}$	Figure 1: Adaptively smoothed 0.3-10 keV Chandra image of Mrk 273 with a smoothing scale of 2 pixels ( $\approx$ 1''). The circle has a radius of 10'' and it is centered at the peak of the hard X-ray emission. The ellipse has a size of $42'' \times 25''$ and a position angle of $13\hbox {$^\circ $ }$ . The bright source visible in the upper left corner is Mrk 273x.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{3558fig2.ps}\end{figure}$	Figure 2: The 4.0-10 keV EPIC-PN spectrum fitted with a simple absorbed power law model ( $\Gamma$ is fixed to 1.9). Residuals are found at Fe K $\alpha$ emission line energy (at about 6.5 keV).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.38cm,clip]{3558fig3.ps}\end{figure}$	Figure 3: A simple absorbed power law model applied to the EPIC-PN spectrum of Mrk 273. Strong residuals (data/model) are clearly present above 4 keV and also between 0.6 and 1 keV.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{3558fig5.ps}\end{figure}$	Figure 5: The EPIC-PN spectrum fitted with two thermal plasma components, a highly absorbed and a less absorbed power law with the same spectral index, plus a narrow Fe K $\alpha$ line at 6.4 keV. The best fit parameters for this model are given in Table 3.
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$\begin{figure} \par\includegraphics[angle=270,width=8.2cm,clip]{3558fig6.ps}\par\end{figure}$	Figure 6: The 0.3-8 keV ACIS-S spectrum of the inner 10'' region fitted with two thermal plasma components, a highly absorbed power law and a narrow Fe K $\alpha$ line at 6.4 keV. The best fit parameters are given in Table 4.
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$\begin{figure} \par\includegraphics[angle=270,width=8.3cm,clip]{3558fig7.ps}\par\end{figure}$	Figure 7: The 0.3-8 keV ACIS-S spectrum of the inner 10'' region fitted with a single thermal plasma component, a highly absorbed and a less absorbed power law with the same spectral index, plus a narrow Fe K $\alpha$ line at 6.4 keV. The best fit parameters are given in Table 4.
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$\begin{figure} \par\includegraphics[angle=270,width=8.1cm,clip]{3558fig8.ps}\end{figure}$	Figure 8: The 0.5-0.9 keV unbinned spectrum of the extended hot gas halo. A single APEC model with a temperature of $0.38\pm 0.04$ keV provides a satisfactory fit.
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