Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{Fi091_f1.ps} \end{figure}$ Figure 1: 2-12 keV RXTE-ASM light curve of 4U 1254-69 at a 1-week time resolution. Data points with errors in excess of 0.2 c s^-1 were excluded from this plot. The horizontal lines in the top indicate the WFC coverage of the source and the vertical lines the bursts detected with the WFC. The long vertical line indicates the time of the superburst.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{Fi091_f2.ps} \end{figure}$ Figure 2: The average 2-28 keV profile over all normal bursts observed from 4U 1254-69, except the one related to the superburst. The dashed line refers to the persistent flux level.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{Fi091_f3.ps} \end{figure}$ Figure 3: Light curves obtained with the WFC on January 9-13, 1999 at 300 s resolution ( top panel) and focused on the burst onset at 2 s resolution ( bottom panel, with vertical line indicating a typical 1 $\sigma$ error). The bandpass is 2-28 keV.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{Fi091_f4.ps} \end{figure}$ Figure 4: Time-resolved spectroscopy of the superburst (right) and the normal type-I precursor burst (left). Note the different y scales in both columns of plots. In the top panels, a dashed line indicates the pre-burst flux level for guiding purposes and solid vertical lines indicate the typical 1 $\sigma$ error. The time resolution of the observed photon flux is 2 s in the left and 300 s in the right panel. In the other panels errors are 1 $\sigma$ values. The 2nd row of panels show the bolometric flux of the black body component. The decreased flux levels near $1.8\times 10^4$ and $7.5\times 10^4$ s are due to dipping activity.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{Fi091_f1.ps} \end{figure}$	Figure 1: 2-12 keV RXTE-ASM light curve of 4U 1254-69 at a 1-week time resolution. Data points with errors in excess of 0.2 c s^-1 were excluded from this plot. The horizontal lines in the top indicate the WFC coverage of the source and the vertical lines the bursts detected with the WFC. The long vertical line indicates the time of the superburst.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{Fi091_f2.ps} \end{figure}$	Figure 2: The average 2-28 keV profile over all normal bursts observed from 4U 1254-69, except the one related to the superburst. The dashed line refers to the persistent flux level.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{Fi091_f3.ps} \end{figure}$	Figure 3: Light curves obtained with the WFC on January 9-13, 1999 at 300 s resolution ( top panel) and focused on the burst onset at 2 s resolution ( bottom panel, with vertical line indicating a typical 1 $\sigma$ error). The bandpass is 2-28 keV.
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