Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[angle=90,width=7.2cm,clip]{8027-fig1.eps} \end{figure}$ Figure 1: EPIC-PN image of LMC X-2, toghether with the XMM/Newton X-ray position (blue circle), the Einstein X-ray position (green circle), the position of the optical couterpart of LMC X-2 (red circle), and the position of the X-ray source according to the ROSAT All Sky Survey (black circle). The circles represent the derived error in the position. The coordinate grid refers to the J2000 equinox.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{8027-fig2.eps} \end{figure}$ Figure 2: PN light curve of LMC X-2. The bin time is 100 s. We plot the count rate versus time (in seconds) from the beginning of the observation.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8027-fig3.eps} \end{figure}$ Figure 3: Color-color diagram of LMC X-2 extracted from PN data. The bin size for each point is 1.2 ks, the error bars are at $90\%$ confidence. With time, the source moves from the bottom left to the top right of the diagram.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{8027-fig4.eps} \end{figure}$ Figure 4: White noise subtracted power density spectrum of LMC X-2. The dashed line represents the best fit power-law $\nu ^{-\gamma }$ with $\gamma =1.4$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8027-fig5.eps} \end{figure}$ Figure 5: Residuals of the blackbody+bremsstrahlung model. The mismatch between the two RGS (red and green) and the EPIC-pn (blue) data below 1.3 keV is evident.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.8cm,clip]{8027-fig6.eps} \end{figure}$ Figure 6: Data with best fit model, consisting of a blackbody and a disk blackbody and relative residuals in units of $\sigma$ for RGS1, RGS2 and PN, respectively. The drops in the RGS1 and RGS2 count rates are due to failing CCDs.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8027-fig7.eps} \end{figure}$ Figure 7: Unfolded spectrum in the region of the O VIII emission line. We show data (dark and light grey for RGS1 and RGS2, respectively) toghether with the total model (continuum + line).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{8027-fig2.eps} \end{figure}$	Figure 2: PN light curve of LMC X-2. The bin time is 100 s. We plot the count rate versus time (in seconds) from the beginning of the observation.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8027-fig3.eps} \end{figure}$	Figure 3: Color-color diagram of LMC X-2 extracted from PN data. The bin size for each point is 1.2 ks, the error bars are at $90\%$ confidence. With time, the source moves from the bottom left to the top right of the diagram.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{8027-fig4.eps} \end{figure}$	Figure 4: White noise subtracted power density spectrum of LMC X-2. The dashed line represents the best fit power-law $\nu ^{-\gamma }$ with $\gamma =1.4$ .
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8027-fig5.eps} \end{figure}$	Figure 5: Residuals of the blackbody+bremsstrahlung model. The mismatch between the two RGS (red and green) and the EPIC-pn (blue) data below 1.3 keV is evident.
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$\begin{figure} \par\includegraphics[angle=270,width=7.8cm,clip]{8027-fig6.eps} \end{figure}$	Figure 6: Data with best fit model, consisting of a blackbody and a disk blackbody and relative residuals in units of $\sigma$ for RGS1, RGS2 and PN, respectively. The drops in the RGS1 and RGS2 count rates are due to failing CCDs.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8027-fig7.eps} \end{figure}$	Figure 7: Unfolded spectrum in the region of the O VIII emission line. We show data (dark and light grey for RGS1 and RGS2, respectively) toghether with the total model (continuum + line).
Open with DEXTER