All Figures

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{6774fig1.ps} \end{figure}$ Figure 1: Upper panel: the blank sky data of Nevalainen et al. (2005) after subtraction of the closed filter data. The black crosses show the data points, used for modeling the Galactic emission and CXB. The blue crosses show the data points excluded from the fit. The best-fit model is shown with the red line. The plotted spectrum is binned by a minimum of 20 000 counts per channel, different from that used in the actual fit (see text). The error bars include the 5% systematic uncertainty used in the analysis. Lower panel: the ratio of the data-to-model values in each channel used in the fit.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{6774fig2.ps} \end{figure}$ Figure 2: Exclusion plot based on the blank sky observations. Bins $2.9{-}3.1~{{\rm keV}}$ and $11.6{-}12.6~{{\rm keV}}$ are excluded.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{6774fig3.eps} \end{figure}$ Figure 3: Dependence of the results on closed filter normalization. Red (solid) and green (long-dashed) lines are the same as in Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{6774fig4.ps} \end{figure}$ Figure 4: Hard band light curve for the UMi observation 0301690401. The crosses show the PN > 10 keV band rate of the full FOV in 1 ks bins. The dashed line shows the average, when excluding first 2 time bins. The dotted line shows the corresponding quiescent value in the co-added blank sky data (Nevalainen et al. 2005).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6774fig5.eps} \end{figure}$ Figure 5: Flux from UMi (obs. ID 0301690401). Energy bins have the width of twice the spectral resolution. Shown are the 1, 2, and 3 $\sigma$ errors. One can see that, above 2 keV, flux in most energy bins is zero within $1\sigma$ limits (blue crosses) and for the rest it is zero within $2\sigma$ limits (green crosses). Similarly, below 2 keV black, cyan and yellow crosses represent 1, 2, and 3 $\sigma$ error correspondingly. The solid black line represents the 3 $\sigma$ upper bound on total flux in a given energy bin, which we use to put the limit on DM parameters.
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In the text

$\begin{figure} \par\includegraphics[width=8.05cm,clip]{6774fig6.eps} \end{figure}$ Figure 6: Exclusion from UMi (red solid line), as compared to LMC (green long-dashed line). The blue short-dashed smooth curve shows hypothetical restrictions from UMi observations with 100 ks exposure.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{6774fig7.eps} \end{figure}$ Figure 7: Results and comparison with previous bounds (a region ofparameter space above a curve is excluded).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6774fig8.eps} \end{figure}$ Figure 8: Restrictions on parameters of any DM particle with the radiative decay width $\Gamma$ , emitting photon of energy $E_\gamma$ . Shaded region is excluded.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{6774fig2.ps} \end{figure}$	Figure 2: Exclusion plot based on the blank sky observations. Bins $2.9{-}3.1~{{\rm keV}}$ and $11.6{-}12.6~{{\rm keV}}$ are excluded.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{6774fig3.eps} \end{figure}$	Figure 3: Dependence of the results on closed filter normalization. Red (solid) and green (long-dashed) lines are the same as in Fig. 2.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{6774fig4.ps} \end{figure}$	Figure 4: Hard band light curve for the UMi observation 0301690401. The crosses show the PN > 10 keV band rate of the full FOV in 1 ks bins. The dashed line shows the average, when excluding first 2 time bins. The dotted line shows the corresponding quiescent value in the co-added blank sky data (Nevalainen et al. 2005).
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$\begin{figure} \par\includegraphics[width=8.05cm,clip]{6774fig6.eps} \end{figure}$	Figure 6: Exclusion from UMi (red solid line), as compared to LMC (green long-dashed line). The blue short-dashed smooth curve shows hypothetical restrictions from UMi observations with 100 ks exposure.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{6774fig7.eps} \end{figure}$	Figure 7: Results and comparison with previous bounds (a region ofparameter space above a curve is excluded).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{6774fig8.eps} \end{figure}$	Figure 8: Restrictions on parameters of any DM particle with the radiative decay width $\Gamma$ , emitting photon of energy $E_\gamma$ . Shaded region is excluded.
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