All Figures

$\begin{figure} \par\includegraphics[width=11.98cm,clip]{6651f1t_CMYK.ps} % \par\vspace*{2mm} \includegraphics[width=11.7cm,clip]{6651f1b_CMYK.ps} %\end{figure}$ Figure 1: INTEGRAL IBIS/ISGRI (20-60 keV) mosaic significance images from the first ( top; total exposure of 234 ks) and second season ( bottom; total exposure of 235 ks), using the Hammer-Aitoff projection. Sources and their names are annotated, except for those in the Galactic Center region. The latter are displayed in Fig. 3. Transients (see Table 1) are indicated in red, the other sources in white. The annotated sources are those which reached a significance higher than 7 in either a single revolution, a season or all seasons together (see Table 3).
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In the text

$\begin{figure} \par\includegraphics[width=11.98cm,clip]{6651f2t_CMYK.ps} % \par\vspace*{3mm} \includegraphics[width=11.68cm,clip]{6651f2b_CMYK.ps} %\end{figure}$ Figure 2: Same as Fig. 1 but for the third season ( top; total exposure of 258 ks) and all seasons together ( bottom; total exposure of 727 ks).
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In the text

$\begin{figure} \par\mbox{ \includegraphics[width=8.5cm,clip]{6651f3tl_CMYK.ps} \... ...pace*{2mm} \includegraphics[width=8.5cm,clip]{6651f3br_CMYK.ps} } \end{figure}$ Figure 3: Same as Figs. 1 and 2, but now zoomed in on the Galactic Center region.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=7.6cm,clip]{6651f4tl_CMYK.ps} \h... ...pace*{4mm} \includegraphics[width=7.6cm,clip]{6651f4br_CMYK.ps} } \end{figure}$ Figure 4: Same as Figs. 1 and 2, but for JEM-X (3-10 keV). The same sources as in Figs. 1 and 3 are annotated except for AX J1749.1-2733, IGR J17475-2822, IGR J17456-2901, GRS 1741.9-2853, KS 1741-293 and GRS 1734-292 (all in the Galactic Center region) for reason of clarity.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{6651f5.ps} \end{figure}$ Figure 5: Relative standard deviation ( $\sigma$ / $\overline {F_{\rm A}}$ ) versus mean flux ( $\overline {F_{\rm A}}$ ) for the 20-60 keV band. The different symbols refer to the different kinds of sources as outlined in Table 1; filled circles: black-hole (candidate) binaries, filled squares: X-ray bursters, filled triangles: other low-mass X-ray binaries, open circles: X-ray pulsars, open squares: miscellaneous sources. 4U 1700-377 is outside the boundaries of the plot.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[angle=-90,width=7cm,clip]{6651f6l.ps} \includegraphics[angle=-90,width=7cm,clip]{6651f6r.ps} } \end{figure}$ Figure 6: INTEGRAL IBIS/ISGRI light curves from the three seasons of the Galactic bulge monitoring program, for the energy ranges 20-60 keV ( left) and 60-150 keV ( right). Shown are the black-hole (candidate) binaries detected during our program: 1E 1740.7-2942, GRS 1758-258, H1743-322, XTE J1817-330, and GRO J1655-40. In the 20-60 keV band, we show for the first two sources the averages per hexagonal dither observation (7 pointings), while for the latter we show single pointing fluxes. The 60-150 keV data points are averages per hexagonal dither observation.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=7cm,clip]{6651f7tl.ps}... ...*{4mm} \includegraphics[angle=-90,width=7cm,clip]{6651f7br.ps} } \end{figure}$ Figure 7: INTEGRAL IBIS/ISGRI light curves (20-60 keV) from the three seasons of the Galactic bulge monitoring program. Shown are the averages per hexagonal dither observation for the following type I X-ray burst sources: upper left: GX 17+2, GX 354-0, H1820-303, and GS 1826-24; upper right: KS 1741-293, MXB 1730-335, XTE J1739-285, and SAX J1747.0-2853; lower left: 1A 1742-294, GX 13+1, 4U 1722-30, and GX 3+1; lower right: SLX 1735-269, GRS 1741.9-2853, SLX 1744-299/300, SLX 1737-282, and XB 1832-330.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{6651f8.ps} \end{figure}$ Figure 8: INTEGRAL IBIS/ISGRI (20-60 keV, top) and JEM-X (3-10 keV, bottom; 10-25 keV, middle) light curves (data from single 1800 s pointings) of GX 354-0.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{6651f9.ps} \end{figure}$ Figure 9: Same as Fig. 8 but for 1A 1742-294.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6.8cm,clip]{6651f10t.ps}\par... ...ce*{2mm} \includegraphics[angle=-90,width=6.8cm,clip]{6651f10b.ps} \end{figure}$ Figure 10: Same as Fig. 7, but showing the following sources: top: (other low-mass X-ray binaries) GX 5-1, GX 349+2, GX 9+1, and 1E 1743.1-2843; middle: (X-ray pulsars) OAO 1657-415, IGRJ 17252-3616, GX 1+4, and 3A 1822-371; bottom: (miscellaneous sources) 4U 1700-377, IGR J17098-3628, IGR J17544-2619, XTE J1818-245, and XTE J1743-363.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{6651f11.ps} \end{figure}$ Figure 11: INTEGRAL IBIS/ISGRI light curves (60-150 keV) from the three seasons of the Galactic bulge monitoring program. Shown are the averages per hexagonal dither observation for the following sources: GS 1826-24, GX 1+4, IGR J17098-3628, and 4U 1700-377.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{6651f12.ps} \end{figure}$ Figure 12: Same as Fig. 8 but for GX 5-1.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=5cm,clip]{6651f13l.ps}... ...e*{2mm} \includegraphics[angle=-90,width=5cm,clip]{6651f13r.ps} } \end{figure}$ Figure 13: Left: 10-25 keV and 20-60 keV intensities versus 3-10 keV intensity for GX 5-1. Middle: Hardness (ratio of the count rates in the 10-25 keV and 3-10 keV bands) versus intensity (3-25 keV) for GX 5-1. Right: Hardness versus intensity (20-60 keV) for GX 5-1.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8cm,clip]{6651f14l_CMYK.ps} \includegraphics[width=8cm,clip]{6651f14r_CMYK.ps} } \end{figure}$ Figure 14: INTEGRAL JEM-X (3-20 keV) ( left) and IBIS/ISGRI (20-60 keV) ( right) mosaic significance images of the Galactic Center region during revolutions 424-429 (April 3-21, 2006; MJD 53828-53846), for a total exposure of 69 ks. Note that the same scales are used as in Figs. 1-4. The annoted sources are those similar to Fig. 3. Clearly, most of the sources are "off'' during that time. With JEM-X only SAX J1747.0-2853, 1A 1742-294 and SLX 1744-299/300 are significantly detected, whereas with IBIS/ISGRI only SLX 1744-299/300 and a source positionally coincident with IGR J17456-2901 are significantly detected. We refer to Sect. 4.3 for a more detailed discussion.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{6651f15t.ps}\par\vspace*{2mm} \includegraphics[angle=-90,width=8cm,clip]{6651f15b.ps} \end{figure}$ Figure 15: INTEGRAL IBIS/ISGRI 20-60 keV light curves of IGR J17453-2853 ( Top) and IGR J17354-3255 ( Bottom) around and during the time of their detection.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{6651f16.ps} \end{figure}$ Figure 16: INTEGRAL JEM-X 3-10 keV ( Top) and 10-25 keV ( Bottom) light curve of IGR J17454-2703 during the third visibility season. Data points are from single pointings whenever the source was within the JEM-X field of view.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{6651f17.ps} \end{figure}$ Figure 17: Top: IBIS/ISGRI 20-60 keV light curve; data points are averages per hexagonal dither observation. Bottom: OMC light curve of the optical counterpart of IGR J17544-2619, i.e., 2MASS J17542527-2619526 (= IOMC 6849000050).
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In the text

$\begin{figure} \par\mbox{ \includegraphics[angle=-90,width=7cm,clip]{6651fa1tl.p... ...*{2mm} \includegraphics[angle=-90,width=7cm,clip]{6651fa1br.ps} } \end{figure}$ Figure A.1: INTEGRAL JEM-X light curves of the Crab during the calibration in revolution 365 ( top left) and IBIS/ISGRI light curves of the Crab during the calibration in revolutions 300 ( top right), 365 ( bottom left) and 422 ( bottom right). Plotted per panel are the two energy bands used: JEM-X 3-10 keV ( panel top), 10-25 keV ( panel bottom), and IBIS/ISGRI 20-60 keV ( panel top), 60-150 keV ( panel bottom).

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{6651fa2.ps} \end{figure}$ Figure A.2: IBIS/ISGRI 20-60 keV ( top) and 60-150 keV ( bottom) Crab count rates as a function of the off-axis angle.

In the text

$\begin{figure} \par\includegraphics[height=.35\textheight,angle=-90]{6651fb1.ps} \end{figure}$ Figure B.1: IBIS/ISGRI 20-60 keV 5 $\sigma$ sensitivity information. We refer to the text (Sect. B) for a detailed explanation of the various data points and curves.

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{6651fc1.ps} \end{figure}$ Figure C.1: Average flux from the mosaic image of all pointings (ScWs) versus the mean flux over all single pointings (20-60 keV). Data are taken from Tables 3 and 6; plotted are those sources which reached a significance higher than 7. The values for which the mosaic average flux equals the mean flux are indicated by a continuous line; the dashed line indicates where the mosaic flux equals 90% of the mean flux.

In the text

$\begin{figure} \par\includegraphics[width=11.98cm,clip]{6651f2t_CMYK.ps} % \par\vspace*{3mm} \includegraphics[width=11.68cm,clip]{6651f2b_CMYK.ps} %\end{figure}$	Figure 2: Same as Fig. 1 but for the third season ( top; total exposure of 258 ks) and all seasons together ( bottom; total exposure of 727 ks).
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$\begin{figure} \par\mbox{ \includegraphics[width=8.5cm,clip]{6651f3tl_CMYK.ps} \... ...pace*{2mm} \includegraphics[width=8.5cm,clip]{6651f3br_CMYK.ps} } \end{figure}$	Figure 3: Same as Figs. 1 and 2, but now zoomed in on the Galactic Center region.
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$\begin{figure} \par\mbox{\includegraphics[width=7.6cm,clip]{6651f4tl_CMYK.ps} \h... ...pace*{4mm} \includegraphics[width=7.6cm,clip]{6651f4br_CMYK.ps} } \end{figure}$	Figure 4: Same as Figs. 1 and 2, but for JEM-X (3-10 keV). The same sources as in Figs. 1 and 3 are annotated except for AX J1749.1-2733, IGR J17475-2822, IGR J17456-2901, GRS 1741.9-2853, KS 1741-293 and GRS 1734-292 (all in the Galactic Center region) for reason of clarity.
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$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{6651f8.ps} \end{figure}$	Figure 8: INTEGRAL IBIS/ISGRI (20-60 keV, top) and JEM-X (3-10 keV, bottom; 10-25 keV, middle) light curves (data from single 1800 s pointings) of GX 354-0.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{6651f9.ps} \end{figure}$	Figure 9: Same as Fig. 8 but for 1A 1742-294.
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$\begin{figure} \par\includegraphics[angle=-90,width=6.8cm,clip]{6651f10t.ps}\par... ...ce*{2mm} \includegraphics[angle=-90,width=6.8cm,clip]{6651f10b.ps} \end{figure}$	Figure 10: Same as Fig. 7, but showing the following sources: top: (other low-mass X-ray binaries) GX 5-1, GX 349+2, GX 9+1, and 1E 1743.1-2843; middle: (X-ray pulsars) OAO 1657-415, IGRJ 17252-3616, GX 1+4, and 3A 1822-371; bottom: (miscellaneous sources) 4U 1700-377, IGR J17098-3628, IGR J17544-2619, XTE J1818-245, and XTE J1743-363.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{6651f11.ps} \end{figure}$	Figure 11: INTEGRAL IBIS/ISGRI light curves (60-150 keV) from the three seasons of the Galactic bulge monitoring program. Shown are the averages per hexagonal dither observation for the following sources: GS 1826-24, GX 1+4, IGR J17098-3628, and 4U 1700-377.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{6651f12.ps} \end{figure}$	Figure 12: Same as Fig. 8 but for GX 5-1.
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$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=5cm,clip]{6651f13l.ps}... ...e*{2mm} \includegraphics[angle=-90,width=5cm,clip]{6651f13r.ps} } \end{figure}$	Figure 13: Left: 10-25 keV and 20-60 keV intensities versus 3-10 keV intensity for GX 5-1. Middle: Hardness (ratio of the count rates in the 10-25 keV and 3-10 keV bands) versus intensity (3-25 keV) for GX 5-1. Right: Hardness versus intensity (20-60 keV) for GX 5-1.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{6651f15t.ps}\par\vspace*{2mm} \includegraphics[angle=-90,width=8cm,clip]{6651f15b.ps} \end{figure}$	Figure 15: INTEGRAL IBIS/ISGRI 20-60 keV light curves of IGR J17453-2853 ( Top) and IGR J17354-3255 ( Bottom) around and during the time of their detection.
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$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{6651f16.ps} \end{figure}$	Figure 16: INTEGRAL JEM-X 3-10 keV ( Top) and 10-25 keV ( Bottom) light curve of IGR J17454-2703 during the third visibility season. Data points are from single pointings whenever the source was within the JEM-X field of view.
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$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{6651f17.ps} \end{figure}$	Figure 17: Top: IBIS/ISGRI 20-60 keV light curve; data points are averages per hexagonal dither observation. Bottom: OMC light curve of the optical counterpart of IGR J17544-2619, i.e., 2MASS J17542527-2619526 (= IOMC 6849000050).
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