All Figures

$\begin{figure} \par\includegraphics[width=9cm,angle=-90,clip]{2314fig1.eps}\end{figure}$ Figure 1: Soft and hard light curves and hardness ratios of WX Pyx for May 2003 PN data.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,angle=-90,clip]{2314fig2.eps}\end{figure}$ Figure 2: Power spectrum for May EPIC-PN observation of WX Pyx. The peaks near $6.4\times 10^{-4}$ are identified as the ${\omega }-{\Omega }$ , ${\omega }$ , and ${\omega }+{\Omega }$ frequency components, respectively. The dashed line is the approximate 3 ${\sigma }$ detection threshold.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,angle=-90,clip]{2314fg3a.eps}\par\vspace*{5mm} \includegraphics[width=5cm,angle=-90,clip]{2314fg3b.eps}\end{figure}$ Figure 3: Normalized X-ray light curves in the ( top) 0.5-2 and ( bottom) 2-10 keV bands and folded at the measured spin period. The normalization factors are soft: 0.0459 cts s^-1 and hard: 0.2013 cts s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=5.25cm,angle=-90,clip]{2314fig4.eps}\end{figure}$ Figure 4: Simultaneous model fit to the EPIC-PN, -MOS1, -MOS2 spectra from the May observation and the EPIC-PN spectrum from the April observation. No credible evidence exists for any Fe emission, or any other lines. The May PN spectrum is uppermost of the stack; the April PN spectrum lies among the MOS spectra. The model shown does not include a line component, so any line emission should appear in the residuals.
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In the text

$\begin{figure} \par\includegraphics[width=5.75cm,angle=-90,clip]{2314fig5.eps}\end{figure}$ Figure 5: Contour plot for the bremsstrahlung temperature and column density $N_{\rm H}$ . The contours correspond to the 1 ${\sigma }$ , 90%, and 99% levels in ${\Delta }{\chi }^2$ for 2 parameters of interest.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,angle=-90,clip]{2314fig1.eps}\end{figure}$	Figure 1: Soft and hard light curves and hardness ratios of WX Pyx for May 2003 PN data.
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$\begin{figure} \par\includegraphics[width=5cm,angle=-90,clip]{2314fig2.eps}\end{figure}$	Figure 2: Power spectrum for May EPIC-PN observation of WX Pyx. The peaks near $6.4\times 10^{-4}$ are identified as the ${\omega }-{\Omega }$ , ${\omega }$ , and ${\omega }+{\Omega }$ frequency components, respectively. The dashed line is the approximate 3 ${\sigma }$ detection threshold.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=5cm,angle=-90,clip]{2314fg3a.eps}\par\vspace*{5mm} \includegraphics[width=5cm,angle=-90,clip]{2314fg3b.eps}\end{figure}$	Figure 3: Normalized X-ray light curves in the ( top) 0.5-2 and ( bottom) 2-10 keV bands and folded at the measured spin period. The normalization factors are soft: 0.0459 cts s^-1 and hard: 0.2013 cts s^-1.
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$\begin{figure} \par\includegraphics[width=5.75cm,angle=-90,clip]{2314fig5.eps}\end{figure}$	Figure 5: Contour plot for the bremsstrahlung temperature and column density $N_{\rm H}$ . The contours correspond to the 1 ${\sigma }$ , 90%, and 99% levels in ${\Delta }{\chi }^2$ for 2 parameters of interest.
Open with DEXTER