All Figures

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6457fig1.eps} \end{figure}$ Figure 1: RXTE/ASM light curve for HETE J1900.1-2455 averaged over 1-day intervals from May 5, 2005 (53500 MJD). The count rate has been converted into flux using 1 Crab Unit for 75 cts s^-1 (Levine et al. 1996). The arrows indicate the times of the detected X-ray bursts (Vanderspek et al. 2005; Barbier et al. 2005; Galloway et al. 2005; and this work).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{6457fig2.ps} \end{figure}$ Figure 2: The unfolded spectrum of HETE J1900.1-2455 fit with a COMPPS model plus a BB and a Gaussian line. The data points correspond to the PCA (3-22 keV), JEM-X (3-22 keV), HEXTE (16-90 keV) and the ISGRI (20-300 keV) spectra, respectively. The blackbody model is shown by a dot-dashed curve, the dotted curve gives the COMPPS model, the dashed curve is the Gaussian line, and the total spectrum is shown by the solid curve. The lower panel shows the residuals between the data and the model.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{6457fig3.ps} \end{figure}$ Figure 3: A bright X-ray burst detected from HETE J1900.1-2455. The JEM-X (3-20 keV, upper panel) and IBIS/ISGRI (18-40 keV; lower panel) net light curves are shown (background subtracted). The time bin is 0.5 s for both IBIS/ISGRI and JEM-X light curve. At high energy the burst shows strong evidence of photospheric radius expansion.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{6457fig4.ps} \end{figure}$ Figure 4: Result of the X-ray burst time-resolved spectral analysis. The apparent blackbody radius was estimated assuming a source distance of 5 kpc.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6457fig1.eps} \end{figure}$	Figure 1: RXTE/ASM light curve for HETE J1900.1-2455 averaged over 1-day intervals from May 5, 2005 (53500 MJD). The count rate has been converted into flux using 1 Crab Unit for 75 cts s^-1 (Levine et al. 1996). The arrows indicate the times of the detected X-ray bursts (Vanderspek et al. 2005; Barbier et al. 2005; Galloway et al. 2005; and this work).
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{6457fig3.ps} \end{figure}$	Figure 3: A bright X-ray burst detected from HETE J1900.1-2455. The JEM-X (3-20 keV, upper panel) and IBIS/ISGRI (18-40 keV; lower panel) net light curves are shown (background subtracted). The time bin is 0.5 s for both IBIS/ISGRI and JEM-X light curve. At high energy the burst shows strong evidence of photospheric radius expansion.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{6457fig4.ps} \end{figure}$	Figure 4: Result of the X-ray burst time-resolved spectral analysis. The apparent blackbody radius was estimated assuming a source distance of 5 kpc.
Open with DEXTER