All Figures

$\begin{figure} \par\includegraphics[angle=90,width=8.7cm,clip]{H4477F1a.ps}\hspace*{6mm} \includegraphics[angle=90,width=8.7cm,clip]{H4477F1b.ps} \end{figure}$ Figure 1: The EPIC PN 0.5-10 keV background subtracted lightcurves of X1254-690 with a binning of 20 s (lower panels) showing a deep dip during the 2001 observation and the lack of dipping activity during the 2002 observation. The upper panels show the hardness ratios (counts between 3-10 keV divided by those between 0.5-3 keV) also with a binning of 20 s. The 0.5-10 keV background counts taken from regions adjacent to the source are also shown. The thick horizontal lines indicate the intervals included in the spectral analysis. The tick mark flags the estimated dip center time chosen as phase 0.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.3cm,clip]{H4477F2.ps} \end{figure}$ Figure 2: A 0.5-10 keV PN background subtracted lightcurve of the dip seen in the 2001 January observation plotted with a time resolution of 4 s showing the rapid intensity variability during the dip. The upper panel shows the hardness ratio (counts between 3-10 keV divided by those between 0.5-3 keV).
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In the text

$\begin{figure} \par\mbox{\includegraphics[height=8.5cm,angle=-90,clip]{H4477F3a.... ...cm} \includegraphics[height=8.4cm,angle=-90,clip]{H4477F3d.ps} } \end{figure}$ Figure 3: The upper panels show the PN spectra of the X1254-690 persistent emission and the best-fit disk-blackbody and power-law continuum models. The residuals (middle panels) reveal the presence of a broad emission feature centered at $\sim$ 0.93 keV, together with narrow absorption features at 6.96 keV and 8.16 keV. The lower panels show the residuals when these features are included in the spectral model.
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In the text

$\begin{figure} \par\includegraphics[width=6.0cm,angle=-90,clip]{H4477F4a.ps}\par... ...0.2cm} \includegraphics[width=6.0cm,angle=-90,clip]{H4477F4b.ps} \end{figure}$ Figure 4: Residuals in the 6.0-9.0 keV energy range when the best-fit models given in Table 1 are fit to the PN spectra of the persistent emission and the normalisations of the narrow absorption features at 6.96 keV and 8.16 keV are set to zero.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.3cm,clip]{H4477F2.ps} \end{figure}$	Figure 2: A 0.5-10 keV PN background subtracted lightcurve of the dip seen in the 2001 January observation plotted with a time resolution of 4 s showing the rapid intensity variability during the dip. The upper panel shows the hardness ratio (counts between 3-10 keV divided by those between 0.5-3 keV).
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$\begin{figure} \par\includegraphics[width=6.0cm,angle=-90,clip]{H4477F4a.ps}\par... ...0.2cm} \includegraphics[width=6.0cm,angle=-90,clip]{H4477F4b.ps} \end{figure}$	Figure 4: Residuals in the 6.0-9.0 keV energy range when the best-fit models given in Table 1 are fit to the PN spectra of the persistent emission and the normalisations of the narrow absorption features at 6.96 keV and 8.16 keV are set to zero.
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