Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{integral11_f1.eps} \end{figure}$ Figure 1: The RXTE/ASM 1.2-12 keV single dwell lightcurve. The starting date in the figure is 2002 Oct. 17, INTEGRAL's launch date. The dashed line shows 2003 March 6, i.e. the date of our first observation. 75 ASM ct/s corresponds to 1 Crab.

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{integral11_f2.eps} \end{figure}$ Figure 2: The IBIS/ISGRI 20-40 keV ( $\sim$ $22^{\circ }$ width and $\sim$ $12^{\circ }$ height) image, showing the location of GRS 1915+105 and three other bright sources in the field, including the new transient IGR J19140+098 discovered during this observation. North is up and East is to the left.

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{integral11_f3.eps} \end{figure}$ Figure 3: The ISGRI 20-40 keV ( top) and 40-80 keV ( bottom) lightcurves. The dashed horizontal lines indicate the 50 mCrab level in the given energy ranges showing, in particular how much steeper the source spectrum is compared to the Crab. The bin size is 2200 s. The time of the observation is given in IJD, or "ISDC Julian Date'', and is defined as the fractional number of days since 2000 Jan. 1 (in other words IJD = JD-2 451 544.5).

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{integral11_f4.eps}\end{figure}$ Figure 4: A SPI 100-200 keV image of GRS 1915+105. GRS 1915+105 is clearly visible at the center of the image (marked). The three other sources seen in Fig. 2 are much fainter in this energy range and not visible.

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{integral11_f5.eps}\vspace*... ...s}\vspace*{2mm} \includegraphics[width=8cm,clip]{integral11_f7.eps}\end{figure}$ Figure 5: The JEM X-2 lightcurves. Top: the whole 100 ks observation showing strong variability. Middle: a zoom covering 1.2 hours. The bin size is 8 s. Bottom: RXTE/PCA color-color diagram. The time bin is 1 s. The scale allows for a direct comparison with Figs. 2a and 2b in Belloni et al. (2000).

In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{integral11_f8.eps}\end{figure}$ Figure 6: The JEM X-2 power spectrum.

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{integral11_f9.eps} \end{figure}$ Figure 7: The JEM X-2 (3-20 keV) and ISGRI (20-450 keV) spectrum. The JEM X-2 spectrum is a mean from $\sim$ 37 min, while the ISGRI spectrum is accumulated over the whole observation of 100 ks. The residuals seen above $\sim$ 300 keV are probably due to the background. No systematics have been included, and the RMF and ARF in the case of ISGRI are preliminary matrices. Calibration is still in progress.

In the text